P. Jenniskens et al. "Radar Enabled Recovery of the Sutter's Mill Meteorite, a Carbonaceous Chondrite Regolith Breccia"

Supplementary Materials:

Table of Content

1. Fall and Recovery

1.1. Trajectory and Orbit..................................................................................................... 2

1.2. Infrasound and Seismic Data........................................................................................ 7

1.3. Doppler Weather Radar Return.................................................................................... 8

1.4. Recovered Samples........................................................................................................ 9

2. Meteorite Characterization

2.1. Reflection Spectroscopy................................................................................................ 14

2.2. Magnetic Characterization........................................................................................... 14

2.3. Petrography and Mineralogy....................................................................................... 16

2.4. Major, Minor, and Trace Element Analyses................................................................ 25

2.5. Sulfur............................................................................................................................ 29

2.6. Highly Siderophile Element Concentrations (Re and Platinum Group Elements)

and Os Isotopes........................................................................................................ 30

2.7. Ultrahigh Precision Cr Isotope Analyses..................................................................... 32

2.8. Oxygen Isotope Analyses.............................................................................................. 36

2.9. C, N, and Ar Isotope Analyses...................................................................................... 41

2.10. Noble Gases (He, Ne, Ar, Kr and Xe)........................................................................ 44

2.11. X-ray Tomography..................................................................................................... 52

2.12. Neutron Tomography................................................................................................. 55

2.13. Cosmogenic Radionuclides........................................................................................ 56

2.14. Ultra-high Resolution Mass Spectroscopy and Nuclear Magnetic Resonance

Spectroscopy........................................................................................................... 58

2.15. Raman Spectroscopy.................................................................................................. 60

2.16. Liquid Chromatography Mass Spectrometry............................................................. 61

2.17. Gas Chromatography Mass Spectrometry................................................................. 63

2.18. Thermoluminescence.................................................................................................. 65

References and Notes only cited in Supporting Materials Section (49-106)................ 67

2

1. Fall and Recovery

1.1. Trajectory and Orbit

The trajectory of the 14:51:12 – 17 UTC, April 22, fireball was calculated (49) based on

photographs taken at Rancho Haven, NV, and two videos at Incline Village, NV, and Brush

Creek, CA. Astrometric data were obtained by matching the foreground features in each image to

those in a similar image containing a star background, taken at a later time. The accuracy of the

star background position and orientation is limited by the image resolution, but also by how

precise foreground features were matched.

Fig. S1. At Rancho Haven, NV, three photographs were obtained within the time span of two seconds by

Lisa Warren from +39º54’24.8”N, 239º59’31.9”E, and 1381m altitude, with a Pentax K200D f = 18 mm

Digital Still Camera. Image shows the second photograph taken. A star background image is overlaid as

photographed on May 24, 2012 at 4h27m21s UTC. Insets show enlargements of the fragment train in

each of the three photographs.

The star background image for the Rancho Haven location (Fig. S1) was taken with the same

camera as the fireball photograph. Small perspective differences remained due to an uncertainty

of the exact location of the observer. The perspective was matched in azimuth to trees furthest in

the field of view. The fireball appeared at a range between 147 and 152 km from the observer.

3

The Lake Tahoe video (Fig. S2) was saved as 352 × 288 pixel sized video frames. The

orientation and scale of the image is fixed by the location of the mountain range and the position

of the moon in twilight at three known points in time. A 64º vertical field of view (0.22º/pixel)

was fitted with an accuracy of about ±1 pixel, but a possible systematic uncertainty of order

0.4º/pixel may exist. The range to the fireball was a short 94 to 105 km. The meteor is first

detected well after fragmentation and is an extended image in each frame. The speed of the

leading fragment was measured. Different parts of the fragment train seemed to end at about the

same altitude.

Fig. S2. At Incline Village, NV, David Lockard provided this HikVision video security camera footage

overlooking Lake Tahoe from +39º14’16.3”N, 240º03’21.6”E, and altitude 1837m. A map of the star

background is overlaid as it would appear on May 8, 2012 at 13h04m UTC.

The Brush Creek video (Fig. S3) has detailed and relatively distant foreground features,

which were matched in azimuth to ~0.3º accuracy, and ~0.1º in elevation. A different GoPro

camera was used to calibrate the image projection, after which the perspective was corrected for

lens projection. Star background images were taken with a different camera, which were then

used to identify the foreground features in Google maps. The estimated observer position may be

off by a few meters. The video shows a steady field, but with some motion jitter. The fireball

was 332 - 337 km from the observer. There is overlap with the Rancho Haven photographs: the

onset of persistent emission (Fig. S1) is visible in the Brush Creek video towards the end.

4

Fig. S3. At Brush Creek near Johnsondale, CA, the fireball was filmed by Shon Bollock

(http://vimeo.com/41031380) with a fixed position GoPro Hero 2 wide angle video camera at 720p (1280

× 720 pixels, 60 frame/s) from 35º58’25.2”N, 241º31’58.2”E, and altitude 1504m. The image was

reprojected in a gnomonic projection. Together with selected frames of the fireball, a map is shown of the

reference star background field at 9h25m00s UT on June 3, 2012.

Fig. S4. Left: the ground-projected fireball trajectory from triangulation of combinations Rancho Haven –

Lake Tahoe (red), Brush Creek – Rancho Haven (blue), and Lake Tahoe – Brush Creek (black). The

position of the blast wave origin derived from seismic measurements is also plotted (o). Right: the

measured velocity along the fireball trajectory.

5

The triangulated trajectories for the combinations Lake Tahoe – Brush Creek (convergence

angle between planes from each site: Q = 71.5º), Rancho Haven – Lake Tahoe (Q = 23.2º), and

Brush Creek – Rancho Haven (Q = 48.4º) show only a small divergence (Fig. S4). They are in

agreement (within uncertainty interval) with the position of the blast wave origin calculated from

seismic records. The velocity profile is constant in the Brush Creek video (Fig. S4), but strong

deceleration is observed towards the end of the trajectory in the Lake Tahoe video.

Fig. S5. The preatmospheric orbit of CM chondrites Sutter’s Mill and Maribo in the solar system (Table

1, main text). Blue is the part of the orbit below the ecliptic plane, red above. γ is towards the direction of

vernal equinox. Planet positions are for 22 April, 2012.

Orbital elements (Table 1, and Fig. S5) were calculated (49) based on the mean radiant

position of all three solutions, using the standard deviation between solutions as a measure of

uncertainty. The orbit prior to entry in Earth’s atmosphere is close to that of a Jupiter Family

comet, with aphelion just inside of Jupiter’s orbit and perihelion near the orbit of Mercury. The

asteroid approached Earth from the sunward direction. One node is at Earth’s orbit, while the

other node is at the orbit of Venus, a feature shared with Maribo (Fig. S5), perhaps because close

encounters with the terrestrial planets can de-couple the orbit from the 3:1 resonance.

6

Table S1 and Fig. S5 compare the Sutter’s Mill entry conditions and preatmospheric orbit to

that of other meteorite falls derived previously from video and/or photographic observations of

the fireball. Sutter’s Mill and Maribo stand out by having a low perihelion distance of 0.45 AU,

with most other falls having values in the range 0.78-1.00 AU. The entry velocity is twice that of

most other falls. The distribution of semimajor axis has two peaks, roughly corresponding to the

3:1 mean-motion resonance (2.5 AU) and the ν6 resonance (2.1 AU).

Table S1. Overview of known meteorite falls with atmospheric trajectory and orbit determinations from photographic and video data (Equinox J2000). Fall Date (UT)

Meteorite name (location) Mv at 100km (magn.)

Initial Velocity (km/s)

Entry Angle (º)

Start Alt. (km)

Peak Alt. (km)

Final Alt. (km)

Final Vel. (km/s)

D (m)

Ekin (kt)

Ref.

4/22/2012 Sutter's Mill (California) -18.3 28.6 26.3 90.2 47.6 30.1 19 3.0 4.0 This 4/13/2010 Mason Gully (Australia) -9.4 14.53 53.9 83.46 35.8 23.84 4.1 0.3 0.001 (50) 9/26/2009 Grimsby (Canada) -14.5 20.91 55.2 100.5 39 19.6 3.1 0.18 0.002 (51) 4/9/2009 Jesenice (Slovenia) -15 13.78 40.6 88 26 15.3 3.0 0.4 0.004 (52) 1/17/2009 Maribo (Denmark) -16.5 28.0 30.2 111.8 58 32 -.- 1.0 0.08 (53-54) 11/21/2008 Buzzard Coulee (Canada) -15 18.0 66.7 86 -.- <17.6 -.- 1.4 0.32 (55) 7/10/2008 Almahata Sitta (Sudan) -20 12.42 20 65 37.5 32.7 -.- 4.1 1.2 (56-57) 7/20/2007 Bunburra Rockhole (Aus.) -9.6 13.36 -.- 62.8 -.- 29.95 5.8 0.3 0.001 (58-59) 1/4/2004 Villalbeto de la Pena (Sp.) -18 16.9 29.0 47 28 22.20 7.8 0.8 0.02 (60) 3/27/2003 Park Forest (Illinois) -21.7 19.5 29 82 28 <18 -.- 1.3 0.5 (61) 4/6/2002 Neuschwanstein (Germ.) -17.2 20.95 49.5 84.95 21 16.04 2.4 0.45 0.026 (62) 5/6/2000 Morávka (Czech Rep.) -20.0 22.5 20.4 80 33 21.2 3.7 1.0 0.1 (63) 1/18/2000 Tagish Lake (Canada) -22 15.8 17.8 -.- 38 31 9 4 1.7 (64) 10/9/1992 Peekskill (New York) -16 14.72 80 3.4 -.- 33.6 -.- 1.2 0.5 (65) 5/7/1991 Benesov (Czech Republic) -19.5 21.0 -.- -.- 34 19 5 1.6 0.2 (66) 2/6/1977 Innisfree (Alberta) -12.1 14.54 67.8 >62 36 21 4.7 0.19 0.0005 (67-68) 1/4/1970 Lost City (Oklahoma) -12 14.15 38 86 28 19.5 3.4 0.3 0.004 (69-70) 4/7/1959 Pribram (Czech Republic) -19.2 20.89 43 98 46 13.3 -.- 1.8 0.5 (62,71) Fall Date (UT)

Meteorite name (location) Type q (AU)

a (AU)

e i (º)

ω (º)

Node (º)

CRE (My)

Mrec (kg)

4/22/2012 Sutter's Mill (California) CM2 0.456 2.59 0.824 2.38 77.8 32.774 0.05 0.94 4/13/2010 Mason Gully (Australia) H5 0.9824 2.470 0.6023 0.832 18.95 203.211 -.- 0.024 9/26/2009 Grimsby (Canada) H4-6 0.9817 2.04 0.518 28.07 159.865 182.956 -.- 0.215 4/9/2009 Jesenice (Slovenia) L6 0.998 1.75 0.43 9.6 190.5 19.2 4 3.6 1/17/2009 Maribo (Denmark)* CM2 0.481 2.34 0.795 0.72 99.0 117.638 ~1 0.026 11/21/2008 Buzzard Coulee (Canada) H4 0.961 1.225 0.215 25.49 212.02 238.937 -.- 41 7/10/2008 Almahata Sitta (Sudan) Ur 0.9000 1.3082 0.4536 2.5422 234.450 194.101 20 11 7/20/2007 Bunburra Rockhole (Aust.) Eu 0.643 0.851 0.245 9.07 209.9 297.595 -.- 0.34 1/4/2004 Villalbeto de la Pena (Sp.) L6 0.860 2.3 0.63 0.0 132.3 283.671 48 5.2 3/27/2003 Park Forest (Illinois) L5 0.811 2.53 0.680 3.2 237.5 6.116 -.- 18 4/6/2002 Neuschwanstein (Germ.) EL6 0.793 2.40 0.670 11.41 241.20 16.827 48 6.2 5/6/2000 Morávka (Czech Rep.) H5 0.982 1.85 0.47 32.2 203.5 46.258 6.7 1.4 1/18/2000 Tagish Lake (Canada) C2 ung 0.884 1.98 0.55 2.0 224.4 297.901 7.8 10 10/9/1992 Peekskill (New York) H6 0.886 1.49 0.41 4.9 308 17.030 32 12.37 5/7/1991 Benešov (Czech Republic) LL3.5 0.9246 2.427 0.6191 23.70 218.67 47.001 -.- 0.009 2/6/1977 Innisfree (Alberta) L5 0.986 1.872 0.473 12.28 177.97 317.52 26 4.58 1/4/1970 Lost City (Oklahoma) H5 0.933 1.66 0.417 11.98 161.00 283.77 8 17.2 4/7/1959 Pribram (Czech Republic) H5 0.7895 2.401 0.6711 10.482 241.75 17.791 12 5.7 *) Orbit calculated from seven Juliusruh radar head-echo detections: January 17, 2009, 19:08:27.50 UT: altitude calculated from range = 111.80 km, azimuth (anti-clock from E) = 347.56º; 19:08:27.57, 110.0 km, 346.18º; 19:08:27.93, 105.45 km, 344.61º; 19:08:29.01, 90.65 km, 182.70º; 19:08:29.15, 87.97 km, 181.08º; 19:08:29.49, 83.69 km, 178.84º; 19:08:29.79, 79.02 km, 177.64º.

7

1.2. Infrasound and Seismic Data

Two infrasound stations detected the infrasound signal from the Sutter's Mill fireball. Both

recorded an unusually long period (Table S2a) signal, normally associated with very large

kiloton (kt) class detonations. The signal period and frequency content of the infrasound signals,

given the relatively large range to the fireball, suggest a source energy >> 0.1 kt. Based on the

period a best fit source energy is 4.0 (-2.2 +3.4) kt of TNT. The underlying theory (5) relates the

observed period to the blast radius, which is a function of speed and diameter of the body. The

uncertainty interval is mostly due to the scatter in the empirical period relationship, precise to

about a factor of two. The small measured difference in period between the two stations is

typical of other falls and usually attributed to the signal coming from different parts of the trail.

A signal coming from a point along the trajectory where fragmentation occurs will give a larger

blast radius and consequently longer period. Additionally, sources located at higher altitudes tend

to produce larger periods for fixed energy release.

The amplitude-based relations do not provide consistent results for Sutter’s Mill, perhaps an

indication of unusual behavior. In particular, the steep topography in Western North America

could lead to caustics and scattering which together with uncertainties in general atmospheric

conditions and propagation introduce large error factors in the final energy estimates from

amplitude alone. Period measurements are much less affected by these effects.

Table S2a. Summary of Sutter’s Mill bolide infrasound signal measurements. The signal measurement methodology is described in (5).

8

Table 2b. Summary of the arrival times of the impulsive phase at seismic stations. Dist.: Distance from

station to source; Az.: Source to station azimuth (surface projection); Ang.: Take off angle, source to

station; Res.: Travel time residual in seconds relative to assumed velocity model; Wt.: Travel time

weighting factor.

Station Lat. Lon. Elev. (m)

Arrival Time

Dist. (km)

Az. (º)

Ang. (º)

Res. (s)

Wt.

EMB 38º58.48' 120º06.17' 2134 14:54:31.13 30.6 31 149 +1.55 0.99 RUB 39º03.10' 120º09.29' 2045 14:54:38.83 36.5 18 145 -0.97 1.00 EBP 38º34.96' 119º48.44' 2432 14:54:59.15 45.2 112 139 +0.18 1.00 TAH 39º09.09' 120º09.78' 2079 14:55:44.63 47.0 13 138 -1.61 0.98 MPK 39º17.57' 120º02.18' 2599 14:54:57.03 65.2 19 128 +1.33 0.99 EGLV 39º09.47' 119º43.24' 1435 14:55:47.90 67.6 46 127 -1.47 0.99 SLID 39º18.86' 119º53.03' 2929 14:56:18.36 72.8 28 125 +0.90 1.00 CMB 38º02.07' 120º23.19' 697 14:56:03.62 78.7 187 123 -0.05 1.00

The source location of the seismic signals, assumed to be a point source, was developed from

first arrivals at 8 seismic stations along the eastern Sierra and in western Nevada (Table 2b).

Seven stations are part of the Nevada seismic network (8). Travel time residuals from one

California station operated by UC Berkeley, station CMB - Columbia College, helped define the

location. The location of the source was calculated from the impulsive arrival in the wave train

by using a half-space sound velocity of 310 m/s (consistent with -25ºC). Impulsive arrivals from

stations to the west and stations to the east did not converge well, possibly due to directivity of

the wave front following the explosion. Also, the wave train is fairly complex, possibly from

multi-pathing of the surface arrival and because many of the stations are on variable topography.

The result is a point source location at +38.7390N, 120.2865W (Fig. S4), with uncertainty of

±5.4 km horizontal error, and an elevation of 54.8 km MSL with ±10.9 km vertical error. The

origin time was April 22, 2012, at 14:51:12.80 ± 1.15 s UTC.

1.3. Doppler Weather Radar Return

Figure S6 shows the progression of the falling meteorites in altitude and time. This plot shows all

radar data from the three nearest NEXRAD radars. Open squares indicate radar sweeps that do

not show evidence of falling meteorites, while solid squares indicate radar sweeps with excess

reflectivity over the Lotus and Coloma area. The first radar reflections were detected at 14:52:10

9

UTC at 16.8 km above ground level by KRGX. These records are shown compared against the

calculated fall curves for a range of meteorite masses, using a dark flight model that calculated

meteorite fall using ambient winds-aloft measurements made by a weather balloon launched

from Reno, NV at 12:00 UTC on the day of the Sutter’s Mill fall.

Fig. S6. Time-altitude relation for radar sweeps that did (solid square) and did not (open square) detect

the falling meteorites. Solid lines are meteorite trajectories for different masses. The total of the absolute

values of all radar reflectivity values bearing meteorite signatures are given in parentheses. Along a given

mass trajectory, the higher that value is, the greater the number of meteorites in that radar sweep.

The radar returns originated predominantly from small 0.1 – 5 g fragments (Fig. S6), even in

areas where larger meteorites were recovered. The presence of small meteorites among larger

ones is confirmed by recovered meteorites (Table S3).

1.4. Recovered Samples

Figure S7 provides images of the various SM stones examined in this study. A complete list of

known recovered SM stones found before June 26, 2012, is provided in Table S3.

10

Fig. S7: (A) Fragments of Sutter’s Mill SM2 with subsample identifications. (B) SM51, an oriented

specimen. (C) SM12, with subsample identifications. (D) SM3, subject of X-ray computed tomography

(CT) study. (E) SM54, subject of X-ray and neutron tomography. (F) SM9, subject of X-ray CT. (G)

SM43, subject of chemical analyses and gamma-ray counting. (H) SM18, subject of gamma-ray counting

and accelerator mass spectrometry analyses of 10Be, 26Al, and 36Cl. (I) SM53 (the main mass thus far).

11

Table S3. Tally of reported finds prior to June 26, 2012. Meteorites marked with an asterisk (*) were

examined for this study. Coordinates between brackets are approximate.

SM# Mass (g) Latitude (N) Longitude (W) Date find Finder (Property owner)

1 5.6 38.8033 120.9075 4/24/2012 Robert Ward

2* 4.0 38.8029 120.9086 4/24/2012 Peter Jenniskens

3* 5.0 38.8103 120.9269 4/25/2012 Brien Cook

4 17.0 38.8040 120.9086 4/26/2012 Brenda Salveson

5 -.- -.- -.- -.- [not a meteorite]

6 2.4 38.8037 120.9049 4/26/2012 Patrick Murphy

7 6.0 38.8065 120.8879 4/27/2012 Jerry Moorman

8 19.0 38.8069 120.9358 4/27/2012 Susan Monroe

9* 6.3 38.8029 120.8928 4/27/2012 Eric Bowker

10 6.2 38.8053 120.9184 4/28/2012 Loraine Logan

11 14.5 38.8071 120.8925 4/28/2012 Tania McAlliser

12* 17.5 38.7857 120.9091 4/29/2012 Moni Waiblinger (Merv de Haas)

13 18.9 38.7938 120.9217 4/29/2012 Marcos & Jennifer

14 11.5 38.8027 120.8945 5/1/2012 Suzanne Matin

15 11.3 38.8069 120.9358 4/27/2012 Mike & Julie Steward

16 15.0 38.8016 120.9078 4/30/2012 Jim & Bailey Plimpton

17 7.2 38.8003 120.8910 4/26/2012 Greg & Abriela Jorgensen

18* 5.4 38.8125 120.9056 5/2/2012 Greg Jorgensen

19* 10.0 38.8161 120.9375 5/3/2012 Alice Butler

20 1.1 38.8054 120.8955 4/27/2012 Richard Garcia

21 1.0 38.8014 120.8852 5/4/2012 Bob Pedersen

22 0.6 38.8024 120.8897 4/27/2012 Paul Gessler

23 1.6 38.8065 120.9102 4/27/2012 Vickie Ly

24 2.1 38.8145 120.9156 4/27/2012 Barbara Broide & Ryan Turner

25 7.3 38.8129 120.9246 4/27/2012 Jason Utas

26 3.5 38.8086 120.9041 4/30/2012 Jason Utas & Michelle Myers

27 35.1 (38.8058 120.9624) 5/5/2012 Mitch Carey

28 4.7 38.8059 120.8952 5/5/2012 Madeleine Hogue

12

29 11.8 -.- -.- 5/1/2012 Joan Johnson

30* 3.5 38.7989 120.8810 5/1/2012 Joyce Matin & Mark Dayton

31 5.9 38.8132 120.9238 5/4/2012 Mark Dayton

32 9.6 38.8096 120.9263 5/1/2012 Doug Klotz

33 8.5 38.8071 120.8964 4/27/2012 Connie Nelson

34 1.6 38.7942 120.9814 5/3/2012 Adam Hamlin

35 0.1 38.7910 120.9781 5/1/2012 Robert Ward

36 22.6 (38.800 120.917) 4/27/2012 Mike Shaw

37 2.8 38.8142 120.9106 5/6/2012 Mike Miller

38 7.0 38.8142 120.9110 5/6/2012 Stanley Wall

39 2.5 38.8044 120.8941 4/27/2012 Mike Miller

40 17.7 38.8224 120.9598 5/5/2012 Keith Mueller

41* 9.3 38.8127 120.9077 5/4/2012 David Johnson

42 1.6 38.8146 120.9162 4/28/2012 Mendy Ouzillou

43* 4.3 38.8097 120.9283 4/29/2012 Sandy VanderPol & Emily

44* 5.5 38.7966 120.9196 5/9/2012 Dennis & Karen Kelleher

45 2.9 38.8047 120.9077 5/10/2012 Alex Wolfgram

46 2.4 38.8167 120.8638 5/4/2012 Rebecca Stuart-G.

47* 10.1 38.8078 120.8997 5/1/2012 Teal Triolo

48* 5.1 38.8147 120.8997 5/12/2012 Kelly Heavin

49 5.9 38.8116 120.9126 5/11/2012 Mike Miller

50 42.4 (38.8085 120.9603) 5/9/2012 Robert Ward

51* 12.3 38.8117 120.8957 5/2/2012 Rick Patrinellis

52 12.8 38.8150 120.9176 5/22/2012 Peter Utas

53 204.6 38.8136 120.9716 5/11/2012 Jeffrey Grant A.

54* 20.2 38.8054 120.9689 5/2/2012 Shane Skogberg

55 20.6 38.8086 120.9523 5/25/2012 Keith Jenkerson

56 7.6 38.8143 120.9217 5/11/2012 Bob Willis

57* 2.8 38.8212 120.8504 5/24/2012 Rick Nelson

58 1.3 38.8172 120.8550 5/26/2012 Sandy Cox

59 1.5 38.8328 120.8761 5/26/2012 Sandy Cox

13

60 4.5 38.8187 120.8795 5/26/2012 Rick Nelson

61* 3.4 38.8271 120.8691 5/26/2012 Rick Nelson

62 1.8 38.8151 120.8817 5/27/2012 Sandy Cox

63 8.3 (38.8061 120.9488) 5/26/2012 Dana Jenkerson

64 22.3 (38.8063 120.9483) 5/27/2012 Keith Jenkerson

65 11.6 38.8102 120.9163 5/30/2012 Philipe de Riemer

66 25.2 (38.8060 120.9500) 5/29/2012 Keith Jenkerson

67* 0.3 38.8082 120.9593 6/17/2012 Beverly Girten (Larry Spies)

68 1.0 38.8187 120.8744 6/8/2012 Connie Nelson

69 27.5 38.8034 120.9494 6/23/2012 Dan & Katrina Siders

70 27.0 38.8010 120.9619 6/30/2012 Glenn Arsenault

71 6.2 38.8123 120.9153 6/24/2012 Roy Karen

72 24.3 (38.8065 120.9461) 5/30/2012 Keith Jenkerson

73* 8.1 38.80785 120.91488 6/24/2012 Aidan & Noel Robinson

74 21.6 38.80784 120.95352 6/7/2012 Joel Kaderka

75 6.9 38.80920 120.90670 5/2/2012 Miquel Leon Contreras

76 8.1 38.80581 120.89448 4/27/2012 Sonny Clary

77 13.5 38.80611 120.96903 5/24/2012 several, incl. Jason Utas

78 14.5 38.80597 120.96894 5/26/2012 several, incl. Jason Utas

Notes: SM2, SM12, and SM67 were provided to the consortium, following donation by the

property owners after being found by volunteers in the concerted volunteer searches

organized by NASA Ames Research Center. Part of SM30 was donated by Joyce Matin.

SM36, SM48, SM57 and SM61 were loaned for study by owners. SM18, SM43, SM51, and

SM 73 were donated in part or acquired from local finders by the University of California at

Davis. SM3 was loaned by Brien Cook. SM9 and SM54 were acquired by the American

Museum of Natural History. SM41 was acquired by the Center for Meteorite Studies at

Arizona State University. SM47 and part of SM1 were acquired by the Field Museum of

Natural History.

14

2. Meteorite Characterization

2.1. Reflection Spectroscopy

Figure S8 combines the reflection spectra (72) measured at Brown University for SM12 over the

0.3 to 5 µm wavelength range. Results are compared to the available astronomical observations

of asteroid 1999 JU3 (73), the current Hayabusa 2 mission target. All data are normalized to 1 at

0.55 µm. The near-IR reflectance slope and the details in the 3-µm O-H stretch vibration band

are found to vary as a function of the surface properties, comparing a naturally broken surface, a

shaved surface, and the reflectance from a powder sample of shavings.

Fig. S8. Reflection spectra measured for SM12 over 0.3 to 5 µm range (solid lines), compared to

astronomical observations of 1999 JU3 shown as black dots (73).

Infrared transmission spectra of SM12 confirm the presence of phyllosilicates as evidenced

by a characteristic Si-O stretching feature near 1000 cm-1, a broad O-H stretching feature

centered near 3400 cm-1, and a narrow structural O-H band at 3680 cm-1.

2.2. Magnetic Characterization

Pure magnetite, in a restricted sub-µm grain size range, is the main magnetic mineral in Sutter’s

Mill, but pyrrhotite ((Fe,Ni)1−xS) contributes substantially to remanence. Sub-µm size magnetite

15

was identified from hysteresis measurements on a Princeton Meas. Corp. Micromag operating in

the Vibrating Sample Magnetometer mode (Mrs/Ms = 0.30, Bc and Bcr of 29 and 52 mT, S ratio

of -0.97; with Mrs meaning saturation remanent magnetization, Ms saturation magnetization, Bc

coercivity, Bcr coercivity of remanence, and S the ratio of remanence in a back field of 0.3 T over

the remanence previously acquired in 3T), identification of Verwey transition at 118 K (Fig. S9,

left), and determination of the maximum unblocking temperature of isothermal remanent

magnetization (IRM) near 580°C (Fig. S9, right). Pyrrhotite (likely the hexagonal ferromagnetic

form) is evidenced by the enhanced unblocking of saturation IRM (SIRM) below 300°C.

Fig. S9. Left: Magnetic susceptibility (arbitrary unit) of SM12 from liquid nitrogen to room temperature

measured using the CSL low temperature cryostat attachment on an Agico Kappabridge MFK1

susceptibility measuring device in Aix-en-Provence. Right: Thermal demagnetization of the saturation

isothermal remanent magnetization (SIRM) of a 2 mg fragment of SM12.

Of eight different Sutter’s Mill stones measured for paleomagnetism using 2G Enterprises

cryogenic magnetometers in Davis and Aix-en-Provence, only two (SM2 and SM73) preserved a

low-intensity natural remanent magnetization (NRM) of presumably extraterrestrial origin. The

others (SM12, 18, 51, 57, 61 and 67) showed intensities close to artificial saturation IRM,

indicative of the application of a high magnetic field (> 100 mT), most likely by contact with

rare earth magnets. Both SM2 and SM73 showed unidirectional behavior in the 20-60 mT range

under alternating field (AF) demagnetization. SM2 (log χ = 4.26) had an NRM/ARM ratio in this

AF range of about 35% whereas for SM73 (log χ = 4.19), this ratio was about 5%. Anhysteretic

remanent magnetization (ARM) was acquired in a 100 mT AF field and a 50 µT DC bias field.

As ARM/IRM is 0.3%, the corresponding NRM/IRM ratios are 1.0 and 0.2 ‰.

16

Table S4. Magnetic susceptibility measurements (χ in 10-9 m3/kg) for the different stones, measured with

a Bartington Magnetic Susceptibility Bridge in Davis (except for SM12 which was measured with the

Agico MFK1 Kappabridge in Aix-en-Provence). The measurements separate into a magnetite-rich and a

magnetite-poor group.

Sample Mass (g) log χ s.d. sample Mass (g) log χ s.d. high group low group SM2 0.50 4.26 0.01 SM51 9.02 4.01 0.01 SM12 0.09 4.18 0.01 SM57 1.71 4.05 0.01 SM18 5.06 4.26 0.01 SM68 0.96 4.04 0.05 SM54-1 15.29 4.32 0.01 -.- -.- -.- -.- SM54-2 4.12 4.30 0.01 -.- -.- -.- SM61 1.84 4.27 0.01 -.- -.- -.- SM67 0.35 4.26 0.01 -.- -.- -.- SM73 8.17 4.19 0.01 -.- -.- -.- average 4.26 ±0.05 average 4.03 ±0.02

2.3. Petrography and Mineralogy

Fig. S10. Slice of SM48, showing both light (blue) and dark (red) clasts. Matrix is identified in orange.

In ordinary chondrite regolith breccias, the clasts are lighter than the matrix (Fig. 2, main text;

Fig. S10, blue), where light clasts are normal material and the dark matrix consists of

comminuted clasts that acquired solar wind gases, carbon, charged-particle tracks, and xenolithic

material (31). Sutter’s Mill also has clasts darker than the matrix (Fig. S10, red), which we infer

to be pieces of mature matrix that have been lithified in the regolith, suggesting the asteroid

surface underwent multiple phases of regolith recycling.

17

A polished thin section of SM51-1 (Figs. S11A,B) was mapped in Mg, Ca, Al, Si, Mn, S, Ni, Fe,

P, Cr, and Na X-rays with a resolution of ~5 µm/pixel using the UH JEOL JXA-8500F field-

emission electron microprobe and operating at 15 kV accelerating voltage, 50 nA beam current,

and ~5 µm beam size. The Mg, Ca, and Al, and Fe, Mn, and Ca, and x-ray maps were combined

using a RGB (red : green : blue) color scheme in Adobe Photoshop software. Objects of interest

were subsequently studied in backscattered electrons using the JXA-8500F equipped with a

energy dispersive spectrometer. Electron microprobe analyses (Tables S5 and S6) of silicates and

phyllosilicates were performed with the JXA-8500F operated at 15 kV accelerating voltage, 15

nA beam current, and ~1 µm beam size using five wavelength spectrometers. Carbonates were

measured at 15 kV accelerating voltage, 5 nA beam current, and ~2 µm beam size using five

wavelength spectrometers. For each element, counting times on both peak and background were

30 sec. Minerals with known chemical compositions were used as standards. Matrix effects were

corrected using PAP procedures (74).

Table S5. Representative electron microprobe analyses (in wt.%) of carbonates in Sutter’s Mill, SM51-1.

mineral CaO MgO FeO MnO SiO2 CO2 total calcite 55.1 0.22 0.76 0.02 0.00 43.9 99.9

dolomite 32.1 16.8 2.8 1.6 0.25 46.5 100.0 dolomite 28.9 17.7 4.1 2.0 0.31 46.6 99.6 dolomite 28.5 16.6 5.0 3.2 0.17 46.2 99.6 dolomite 28.9 15.1 5.6 4.1 0.11 45.7 99.6 dolomite 27.8 14.8 5.4 5.7 0.68 45.6 100.1

Table S6. Electron microprobe analyses (in wt.%) of phyllosilicates in Sutter’s Mill, SM51-1.

Location SiO2 TiO2 Al2O3 Cr2O3 FeO

MnO

MgO

CaO Na2O K2O total chondrule phenocryst

avr (n=12) 38.7 0.07 2.5 0.65 15.2 0.18 26.1 0.11 0.37 0.06 84.0

pseudomorphs stdev 2.6 0.03 0.5 0.29 1.4 0.04 2.8 0.06 0.11 0.02 5.5 chondrule mesostasis

avr (n=7) 32.7 0.15 4.7 0.64 30.9 0.24 20.1 0.04 0.58 0.05 90.1

pseudomorphs stdev 1.8 0.01 1.3 0.13 4.0 0.04 2.8 0.02 0.12 0.01 2.1

matrix avr

(n=4) 40.0 0.12 2.5 0.45 14.8 0.22 28.6 0.05 0.28 0.04 87.1 stdev 0.5 0.04 0.1 0.04 0.4 0.03 0.9 0.05 0.03 0.01 0.9 rims around carbonates

avr (n=15) 39.6 0.09 2.5 0.39 14.7 0.22 26.9 0.69 0.30 0.05 85.4

grains stdev 1.0 0.03 0.1 0.05 2.1 0.02 1.1 1.0 0.06 0.01 2.4

18

Fig. S11A. Backscattered electron images

of (A, B) barred olivine chondrule replaced

by ferroan and magnesian phyllosilicates

(phyl), and (C) pyrrhotite (po), pentlandite

(pnt), and magnetite (mgt) in matrix of

Sutter’s Mill, SM51-1.

Fig. S11B. Backscattered electron images of

incompletely aqueously altered (A) calcium-aluminum-

rich inclusion, (B) amoeboid olivine aggregate (C), and

(D) magnesian porphyritic chondrule in the CM2.1

lithology of Sutter’s Mill, SM51-1. cpx = high-Ca

pyroxene; fo = forsterite; phyl = phyllosilicates; ol =

ferromagnesian olivine; pv = perovskite; px = low-Ca

pyroxene; sp = spinel.

19

Subsample SM51-1, consists of two distinct CM2 lithologies, CM2.0 and CM2.1, with a

sharp boundary between them (Fig. 2b, main text). The CM2.0 lithology contains completely

hydrated pseudomorphs after chondrules and refractory inclusions. In addition, the CM2.1

lithology contains rare relict grains (mostly olivine) of incompletely altered type I (Fa0.5−2) and

type II (Fa27−46) chondrules, amoeboid olivine aggregates (AOA), and CAIs. Both lithologies

contain coarse dolomite ((Ca,Mg,Fe,Mn)CO3) and calcite (CaCO3), and hydrated matrix.

Calcite grains are compositionally uniform (Fig. S12) and contain 0.7−1.5 wt.% FeO and

<0.6 wt.% MnO and MgO; dolomite grains are often chemically-zoned and contain 2.6−6.7 wt.%

FeO and 1.5−5.7 wt.% MnO. Phyllosilicates are close to serpentine solid solution.

Fig. S12. Chemical compositions of calcite (cal) and dolomite (dol) in Sutter’s Mill, SM51-1.

For sample SM47, we collected high-resolution backscattered electron (~1 µm/pixel) and

elemental X-ray (~4 µm/pixel) maps (C, O, Mg, Al, Si, S, Ca, Ti, Cr, Fe, Ni) in order to identify

the petrologic components of the meteorite. A 6.9×4.6 mm polished section of Sutter’s Mill

(SM47-1; Field Museum specimen number Me 5799) was analyzed with the University of

Chicago JEOL JSM-5800LV scanning electron microscope equipped with an Oxford/Link ISIS-

300 X-ray microanalysis system. The specimen was embedded in Buehler UHV-compatible

epoxy and polished with diamond lapping film with high purity isopropanol with a nominal

water concentration of <0.05% (in order to minimize loss of water soluble minerals).

20

Fig. S13A. Backscattered electron (BSE) mosaic map of SM47.

21

Fig. S13B. Elemental X-ray maps of polished section SM47. The first image combines Magnesium (Mg,

red), Calcium (Ca, green), and Aluminum (Al, blue), the second Iron (Fe, red), Nickel (Ni, green), and

Sulfur (S, blue). Subsequent maps show individual elements.

22

Unprocessed images from the Oxford ISIS software were stitched together using the

Grid/Collection Stitching plug-in within the freely available Fiji image-processing program. Fiji

automatically stitched and blended the Mg map. The coordinates of each panel within the Mg

photomontage were used to construct all the other element photomontages, so all the element

maps are correctly registered relative to one another.

In SM47-1, unlike in other sections, no carbonate or sulfide veins are observed, but grains of

sulfides and angular calcite are abundant. Single grains of olivine, some of them strongly zoned

(Fa14–63), pyroxene, troilite and pentlandite are abundant, but chondrules are sparse and are

heavily altered (Fig. S13A). Mesostases in three chondrules examined thus far have been

converted to Fe-rich phyllosilicate, and this material encloses olivine pseudomorphs – an FeO-,

Al2O3-, S-bearing material (or intergrowth) that has preserved the shapes of the olivine grains. In

contrast, isolated grains of fresh, nearly FeO-free olivine, pyroxene, and spinel can be found in

the matrix. Refractory inclusions are sparse and small. We found seven small CAIs that are rich

in Mg-Al spinel with minor perovskite±Fe-silicate. They are typically rounded and 20 - 30 µm

across, with outer rims of Fe-silicate. Two have lost their cores, possibly during section

preparation, and are hollow shells of spinel. Spinel grains are typically ~5 µm across, and

perovskite is ~1 µm. An isolated fragment of hibonite ~6 µm across, with ~1.6 wt.% TiO2, is

also present in the section (Fig. S13B).

Synchrotron X-ray Diffraction (S-XRD)

We collected Laue patterns of selected matrix and CaS grains from sample SM2-5 (Fig. S7) by

the Laue synchrotron X-ray diffraction (S-XRD) using the intense X-ray source of SPring-8 in

Japan. At SPring-8 beam line 37XU an undulator is installed and its radiation is further

monochromatized using a Si (111) double-crystal monochromator. The X-ray energy is

automatically adjusted by changing the undulator gap and the angle of a monochromator.

Diffraction patterns are collected on the two-dimensional detector (CMOS Flat panel

detector, Hamamatsu Photonics K.K.). The samples are attached to a XYZ-stage, and the target

micro area in the sample was adjusted on the micro-beam position under an optical microscope.

We applied energies from 30.00 to 20.00 keV (λ = 0.4133−0.6199 Å) at increments of 40 eV

with each exposure time being 0.5 seconds.

23

Fig. S14. Electron backscattered (BSE) images of the thermally metamorphosed CM lithology in sample

SM2. A) A mosaic of an entire section. B) An aggregate consisting of platy enstatite crystals. C) An

extremely embayed forsterite grain. D) A layered CAI, which is typical of CM chondrites. E) Lithic

fragment with a rim of troilite crystals. F) a flaky matrix grain which is a pseudomorph of olivine after

serpentine.

The instrument parameters were calculated from the coordinates on the Debye-Scherrer rings

in the diffraction pattern of Si powder (NIST 640c) taken at 30 keV and the values were used for

further analysis. Normally a Laue pattern records diffraction from a single crystal. However, in

these instances the samples proved to be polycrystalline to a very fine scale, and so powder

patterns were collected. Two patterns of SM2 matrix from the lithology that resembles CM2

chondrites (Fig. S14A) could be successfully indexed as olivine. This was despite the fact that

the morphology of these samples was identical to the flaky serpentine characteristic of CM2

chondrites.

24

Fig. S15. Electron backscattered (BSE) images of the finely comminuted lithology in sample SM2,

which contains minerals typical of reduced meteorites. A) A mosaic of an entire section. B) A vein of

platy Fe-Ni-Ti phosphides and sulfides. C) An embayed grain of oldhamite (CaS) shaped like the letter

“L”. D) Troilite (medium grey) contains fine disseminated phosphide crystals.

We conclude that this particular sample has been heated to at least 500°C, the minimum

temperature necessary to convert serpentine and cronstedtite to olivine (30). This temperature is

also sufficient to convert tochilinite to troilite, which we observe in abundance in matrix and

rimming chondrules and matrix components (Fig. S14), where one would normally observe

tochilinite. A powder Laue pattern of the CaS from the fine-grained SM2 lithology (Fig. S15)

proved to index uniquely as oldhamite (Fig. S16).

25

Fig. S16. Laue XRD pattern of the sample SM2 oldhamite, compare to a calculated oldhamite XRD

pattern.

2.4. Major, Minor, and Trace Element Analyses

X-ray fluorescence (XRF)

The whole-rock sample SM51 was analyzed for element concentrations using a Bruker S8 WD-

XRF at Lawrence Livermore National Laboratory. Analyses were performed on two flat cut

surfaces of the sample using the Bruker QuantExpress analytical program. The instrument

calibration was performed by measuring standard silicate glass discs (Breitländer GmbH),

certified for a suite of major and trace elements, under the same operating conditions as the

samples. All elements from sodium to uranium were analyzed, but only elements measured

above detection limits are reported in Table S7. Detection limits were typically on the order of

50−200 ppm. Typical analytical sum totals were 92−95%; results were normalized to 100%, after

including 2.5% percent concentration of carbon (see Tables S7, S13, S24 and section 2.9). Iron is

reported as Fe2+.

26

Synchotron-induced X-ray Fluorescence (S-XRF)

Sutter’s Mill sample SM51 and a portion of the Murchison (CM) meteorite were analyzed by

synchrotron-induced X-ray fluorescence (S-XRF) (75,76) at the UC Davis DELTA Group X-ray

milliprobe at beam line 2.2 of the Stanford Synchrotron Radiation Lightsource, Stanford Linear

Accelerator Center. Each sample had been cut to expose a flat surface which was exposed to a

3×2 mm2 beam of monochromatic 38 keV polarized X-rays. Repeated measurements were first

made to establish precision, and then the beam was moved in mm steps, totaling 9 measurements

for SM51 and 4 for the Murchison fragment. Mean precision for all measurements was ±8% for

SM51, ±4% for Murchison. Data were collected by a high count rate VORTEX Si(Li) X-ray

detector using 2040−20 eV steps on the 40 keV scale and were reduced using the program

WinAXIL. The spectra were examined for elements from silicon to barium, and then tantalum

through bismuth, 52 elements in all, eliminating noble gases and radioactive elements other than

thorium and uranium. The published data on the Murchison meteorite (cf. 43) were used to

establish the yield and self-absorption corrections, which were then applied to the SM51 data to

obtain mass fraction data in % or ppm. This was made possible by the very close compositional

agreement between the two fragments.

The results for major, minor and trace element compositions of the Sutter's Mill meteorite are

summarized below in Table S7; data lacking statistical significance are excluded.

Notes to Table S7: # Concentrations of carbon and nitrogen are measured separately by different technique (see

details below in Sections 2.9 and 2.16 and Tables S13, S14, S22);

* Concentration of sulfur is measured separately (see details in section 2.5 on Sulfur).

27

Table S7. Major, minor and trace element compositions of the Sutter’s Mill meteorite.

ICP-MS ID-TIMS /ICP-MS

UC Davis (HR ICP-MS)

Fordham (Q-ICP-MS) UMd Element Units

S-XRF (SLAC) SM51

XRF (LLNL) SM51

Average (SM51) (n)

Average (SM2) (n)

Average (SM51) (n)

H                                      He               See  Table  S15                      Li   ppm           1.66   4   1.70   2          Be   ppm           0.044   6                  B     ppm                                  C   wt.%           2.5  #                      N   ppm           559  #                      O                                      F                                      Ne               See  Table  S15                      Na   wt.%       0.47   0.57   4                  Mg   wt.%       13.79   12.67   4                  Al   wt.%       1.34   1.27   4                  Si   wt.%   13.45   13.72                          P   wt.%   0.11   0.13                          S     wt.%   3.14   2.77   3.16*   3                  Cl   ppm   674   700                          Ar                 See  Table  S16                      K   ppm   363                              Ca   wt.%   1.44   2.11   1.41  -­‐  1.82   4                  Sc   ppm           9.23   10   8.39   2          Ti     wt.%   0.056   0.07   0.07   4   0.07   2          V   ppm   81       77.15   4   74.00   2          Cr   wt.%   0.32   0.34   0.31   4                  Mn   wt.%   0.17   0.19   0.18   4   0.19   2          Fe   wt.%   22.2   22.78   22.37   4                  Co   ppm   585   450   560.90   4   590.00   2          Ni   wt.%   1.28   1.29   1.24   4                  Cu   ppm   135   200   152.70   10   159.00   2          Zn   ppm   187   250   212.40   10                  Ga   ppm           9.53   6   9.30   2          Ge   ppm   37.5       33.40   2                  As   ppm                   1.70   2          Se   ppm   15.2               13.00   2          Br       1.9                              Kr             See  Table  S16                      Rb   ppm           1.85   4   2.60   2          Sr   ppm   10.6     10.82   4   9.40   2      Y   ppm   2.1     2.42   4   2.60   2      

28

Table S7 (cont.). Major, minor and trace element compositions of Sutter’ Mill meteorites

Zr   ppm   7.6           4   7.90   2          Nb   ppm           0.494   4   0.480   2          Mo   ppm                    1.107      Ru   ppm   0.93                       0.886   2  Rh   ppm   0.17                              Pd   ppm   0.66       0.860   2    0.650   2    0.652   2  Ag   ppm   0.15                              In   ppm   0.05       0.063   4                  Sn   ppm           1.35   4   0.990   2          Sb   ppm   0.14       0.120   2   0.170   2          Te   ppm   1.5       1.42   2   1.55   2          I     ppm   0.26                              Xe               See  Table  S17                      Cs   ppm   0.13       0.14   4   0.216   2          Ba   ppm           3.28   4   3.28   2          La   ppm           0.373   6   0.408   2          Ce   ppm           0.859   4   1.05   2          Pr   ppm           0.129   4   0.156   2          Nd   ppm           0.677   4   0.714   2          Sm   ppm           0.223   4   0.237   2          Eu   ppm           0.071   10   0.084   2          Gd   ppm           0.172   4   0.314   2          Tb   ppm           0.045   10   0.061   2          Dy   ppm           0.410   10   0.318   2          Ho   ppm           0.083   4   0.080   2          Er   ppm           0.230   4   0.241   2          Tm   ppm           0.041   4   0.042   2          Yb   ppm           0.249   4   0.237   2          Lu   ppm           0.040   8   0.043   2          Hf   ppm           0.143   4   0.180   2          Ta   ppm   0.02       0.021   4                  W   ppm           0.129   4   0.120   2          Re   ppm                   0.054   2   0.0524   2  Os   ppm                           0.607   2  Ir   ppm           0.650   2   0.670   2   0.592   2  Pt   ppm           1.30   2   0.915   2   1.142   2  Au   ppm   0.15                              Hg   ppm                                  Tl   ppm   0.09       0.096   6                  Pb   ppm   1.88       1.61   4                  Bi   ppm           0.069   4                  Th   ppm           0.047   4   0.050   2          U   ppm           0.013   4   0.013   2          

29

HR-ICP-MS and Q-ICP-MS

For wet chemical analyses by ICP-MS techniques, about ~0.4 g and ~1.1 g sample fragments

were obtained from SM43 and SM51 respectively. Fusion crusts were carefully removed, ca.

~0.15 g and ~0.46 g of fresh fragments were further crushed to obtain homogeneous sample

powders for elemental and isotopic measurements.

About 30 mg aliquots from whole rock powders were dissolved in a concentrated HF-HNO3

mixture, and heated in the oven using stainless steel bombs at 190°C for >60 hours.

Approximately 2% (0.5 mg) of each sample was used for major, minor and trace element

abundance measurements, respectively, using the Element XR HR-ICP-MS at University of

California at Davis, which offers the possibility to run some elements at higher resolution to

avoid potential isobaric interferences. Concentrations were calculated by calibrating to a series of

known rock standards. Limits of detection (3σ standard deviation of background) vary

depending on the element in question; REE’s were in the ppq (10-15) level while higher blank

elements such as Na, B, Ni, Cu, Zn, Mg, and Ca were ~0.1−0.5 ppb. Accuracy was assessed by

running a number of known meteorite samples Murchison (CM2), Allende (CV3), Tagish Lake

(ungrouped), Orgueil (CI1), and Lancé (CO3), and comparing our data with published values.

In addition, we used the methods outlined in (29) with a Thermo X Series II ICPMS at

Fordham University, to quantify 45 trace elements by ICPMS. A 30 mg chip of SM2, free of

fusion crust, was split in two, yielding nearly identical results. The results are summarized in

Table S7.

2.5. Sulfur

Sulfur concentrations were measured separately by high resolution inductively coupled plasma

mass spectrometer at Rice University. Three aliquots of 2 mg each (SM51), weighed to a

precision of 0.1% were dissolved in aqua regia for 24 h at 150°C. Resulting solutions were

centrifuged and then diluted into 2 wt.% HNO3, which was then introduced into the mass

spectrometer using a 100 microliter Teflon nebulizer coupled to a cyclonic spray chamber.

Isobaric interferences were resolved under medium mass resolution mode (3000). Three

isotopes were measured (32S, 33S, 34S). Signals were converted to concentrations using two

independent gravimetric standards made from pure anhydrite. Accuracy of gravimetric standards

30

is <1%. External standards ranging from 0.1 ppb to 100 ppm in solution were determined in

order to bracket sample unknowns. Elemental concentrations determined from 32S, 33S, and 34S

agreed to within 1%. External reproducibility was <1%. For meteorite samples, procedural

blanks and memory on the ICP-MS were negligible.

2.6. Highly Siderophile Element Concentrations (Re and Platinum Group Elements) and Os

Isotopes

Two aliquots of approximately 50 mg each of the meteorite powders (SM51-A and SM51-B),

originally prepared from ~0.5 fresh interior piece of SM51, were analyzed at the UMd for highly

siderophile element concentrations (HSE: Re, Os, Ir, Pt, Ru, Pd) and 187Os/188Os isotopic

composition using standard high temperature acid digestion, chemical purification and mass

spectrometry techniques (27, 77). The results are listed in Table S8.

Table S8: Highly siderophile element concentrations and Re-Os isotope systematics. Re

(ppb) Os (ppb)

Ir (ppb)

Ru (ppb)

Pt (ppb)

Pd (ppb)

187Os/188Os 2σ 187Re/188Os 2σ 187Os/188Os initial

Model Age (Ga)

SM 51-A

53.49 600.7 591.0 884.2 1140 651.2 0.12602 0.0001 0.4289 0.0005 0.0921 4.14

SM 51-B

51.31 613.5 593.4 887.0 1143 653.0 0.12613 0.0001 0.4028 0.0005 0.0943 4.41

The Os isotopic compositions of the two aliquots are identical within uncertainties of ±0.1%

(Table S8), and the average ratio of 0.1261 is well within the range of other carbonaceous

chondrites (Fig. S17). Fig. S18 shows CI (Orgueil)-normalized HSE element abundance patterns

for Sutter’s Mill (SM51), compared with data for three other CM chondrites. For the two pieces,

most HSE concentrations are in agreement within 0.4% of one another, consistent with

homogeneity of the finely ground powders. In contrast, Re and Os concentrations differ by 4 and

2%, respectively. These variations are well above the 0.1% analytical reproducibility of these

elements for standards, and indicate moderate heterogeneity between the two powder aliquots.

Further, the resulting calculated 187Re/188Os ratios differ by 6%, and initial 187Os/188Os ratios

calculated for 4.567 Gy are 0.09211 (SM51-A) and 0.09427 (SM51-B). These calculated initial

ratios are significantly lower than current estimates for the initial Solar System 187Os/188Os ratio

at the time of its formation (0.0953). The differences can’t be attributed to nucleosynthetic

31

anomalies in bulk chondrites, as Os isotopic variations are unknown for bulk chondrites, even on

a much smaller scale. In addition, there is no evidence of nucleosynthetic anomalies of a similar

magnitude for neighboring elements in the bulk meteorite.

Fig. S17. 187Re-188Os versus 187Os/188Os plot

showing the data for the two pieces of

Sutter’s Mill examined here, compared with

data for other carbonaceous, ordinary and

enstatite chondrite group. Chondrite data are

from (78). The offsets of the Sutter’s Mill

data from the 4.57 Gy reference isochron is

observed in numerous other chondritic

meteorites.

Thus, given the virtually identical Os

isotopic compositions in the two aliquots,

the differences in Re and Os

concentrations, and especially the 187Re/188Os ratio, must reflect mobility of Re, and to a lesser

degree of Os, as a consequence of some post-formation, open-system behavior of these two

elements. Model ages of 4.14 Gy (aliquot A) and 4.41 Gy (aliquot B) can be interpreted as

reflecting resetting events within the first several hundred million years following formation, as

may result from impact related shock. However, these ages are substantially younger than the

aqueous alteration ages of ~4.563 Gy, defined by the 53Mn-53Cr ages of calcite and dolomite

present in CM chondrites, e.g. (79,80). If the differences are the result of shock during the early

stage of solar system evolution, the disparity between the two ages requires the open-system

behavior to have occurred on a sufficiently small scale, such that powdering the meteorite did not

homogenize the isotopic systematics. This seems unlikely.

Alternately, the analytically indistinguishable Os isotopic compositions of the two pieces

permit an interpretation of recent, open-system behavior. This could have occurred as a result of

the impact event that liberated the meteorite from its parent body. It is even possible that the

single rain event on April 25, experienced by the piece of meteorite from which the powders

were prepared, resulted in the re-distribution of Re within the meteorite, leading to the open-

32

system behavior. Evaluation of pristine and variably altered samples will be required to assess

this possibility. Fig. S-17 illustrates that many chondrites are characterized by open-system Re-

Os isotopic systematics to a similar degree. This has been previously attributed primarily to

terrestrial weathering (77).

Fig. S18. Highly Siderophile Elemental (HSE) pattern normalized to CI (Orgueil). Note that the y-axis in

panel (a) is in logarithmic scale, and in panel (b) is in linear scale, in which the relative differences

between the meteorites are more clearly seen. In addition to Sutter’s Mill (SM51A and B), a few

additional type specimens of CM chondrites (Mighei, Murray and Murchison) are also shown for

comparison. Data for Orgueil and the CM chondrites are from ref. 77.

2.7. Ultrahigh Precision Cr Isotope Analyses

Powdered samples of 30.87 mg (SM43) and 30.12 mg (SM51) were dissolved using

concentrated HF-HNO3 mixture in Teflon capsules sealed in stainless steel bombs and heated in

the oven at 190 °C for 60 hours to make clear solutions. The sample solutions were evaporated,

dissolved in 6 mol L-1 HCl, heated at 90 °C overnight and evaporated again. These samples were

re-dissolved in 6 mol L-1 HCl and about 30% of the sample aliquots were taken for Cr isotope

measurements. Chemical separations were achieved by cation and anion exchange resins to

eliminate Cr from other major and minor elements.

Cr isotopes were determined using Thermo TRITON-plus thermal ionization mass

spectrometer (TIMS) in a static mode at the Department of Geology, University of California,

Davis. In order to minimize the effect of residual mass fractionation, a relatively large number of

repeated measurements were made for each sample (4 sets of 300 ratios, 8 second integration

33

time). About 3 µg Cr was mixed with 3 µL of silica gel-boric acid-Al type activator, and loaded

onto a single W filament. All samples were bracketed by a Cr standard, SRM 979. Four

filaments were prepared for each sample and standard, and two filaments for the standard were

set before and after the four filaments for each sample. The instrumental mass fractionation

effect was corrected according to an exponential law using a 50Cr/52Cr ratio = 0.051859 (81).

Interferences from 50V and 54Fe were also corrected by monitoring 51V and 56Fe. The beam

intensity of 52Cr was set at 1 × 10-10 A (± 15%). A gain calibration and 60-s baseline were

performed before each analysis and amplifiers were rotated for each block. Analytical

procedures for chemical separation and isotope measurement of Cr are discussed more detail in

(82).

Table S9. Cr isotopic data of Sutter’s Mill meteorite (SM43, SM51) and Murchison measured in this

study.

µ53Cr ε54Cr

Sutter’s Mill (SM 43) 14 ± 4 0.95 ± 0.09

Sutter’s Mill (SM 51) 12 ± 4 0.88 ± 0.07

Murchison (CM2) 16 ± 4 0.89 ± 0.08

Murchison (28) 12 ± 4 0.89 ± 0.09

Notes: Reference values of Murchison are from (28). The µ53Cr and ε54Cr values of the sample

were calculated relative to the average of the standards (µ53Cr = [(53,54Cr/52Cr)sample /

(53,54Cr/52Cr)standard -1] × 106), ε54Cr = [(53,54Cr/52Cr)sample/(53,54Cr/52Cr)standard -1] × 104).

In this study, Cr isotopic analysis was also processed for Murchison (CM2), the same whole

rock powder used in (28). The Cr isotopic values of Murchison measured in this study were

identical to those of (28), suggesting that our Cr isotope measurements are reliable.

As shown in Table S9, both 53Cr/52Cr and 54Cr/52Cr ratios were reproduced between the two

stones of SM43 and SM51, and identical within 4 ppm and 9 ppm uncertainties, respectively, at

95% confidence level to that of Murchison reported by Yin et al. (28) and reproduced here.

Given the complex and heterogeneous nature of the Sutter’s Mill meteorite observed in its

petrography and mineralogy, it is surprising that two random subsamples from a regolith breccia

would give identical Cr isotopic composition to the 7th decimal point and similarly so for

34

Murchison. Clearly, Sutter’s Mill and Murchison (and other CM chondrites by inference) sample

a chemical reservoir in the early solar nebula where the Cr isotope composition was fully

homogenized, and subsequently locked into the minerals and stones of Sutter’s Mill and other

CM chondrites.

A key question is, how and when did these diverse components observed in carbonaceous

chondrites, and Sutter’s Mill in particular, come together? How can we devise a tool to date the

formation of bulk carbonaceous chondrites (and their parent bodies)? Note that manganese (Mn)

is a moderately volatile element, and Cr is a relatively refractory element (Fig. 3, main text). Mn

is thus concentrated in the low-temperature matrices of the carbonaceous chondrites, whereas Cr

is relatively concentrated in the refractory components (chondrules and CAIs). Depletion of

moderately volatile elements is a general feature of terrestrial planets and asteroids (83,84). It is

well established that different carbonaceous chondrite groups show a systematic and progressive

depletion pattern for moderately volatile elements, e.g., Mn/Cr (84,85); the Mn/Cr ratio is

governed by the matrix fraction in each chondrite group. This fact allows us to apply 53Mn-53Cr

chronometry, where 53Mn decays to 53Cr with a half-life of 3.7 My, to constrain the timescale of

accretion and compaction of the carbonaceous chondrite parent bodies (28,86).

Fig. S19. 53Mn-53Cr fossil isochron

diagram. Black solid circle is SM43 from

this study. Solid blue squares are bulk

carbonaceous chondrites and solid red

circles are Allende chondrules (28).

As shown in Fig. S19, Sutter’s Mill plots on the systematic trend where the 55Mn/52Cr ratio

correlates with µ53Cr for a group of carbonaceous chondrites (blue squares, which include CI,

35

CM, CV, CR, and Tagish Lake) and Allende (CV) chondrules (red solid circles) (28). The slope

of this “fossil” isochron gives a 53Mn/55Mn ratio of (5.90±0.67) × 10-6.

The precise age of basaltic angrite D’Orbigny allows consistent linking of the 53Mn–53Cr and

other extinct nuclide chronometers to the absolute time scale. D’Orbigny has a most precise 53Mn/55Mn ratio = (3.24±0.04) × 10-6 (87,88). The absolute Pb–Pb age for the D’Orbigny angrite

is refined to be 4,563.37±0.25 My based on the new U isotope composition (89,90).

Fig. S20. Diagram of ε54Cr excess versus Δ17O excess (for definition see Eq. S1 below) among different

carbonaceous chondrites. Data sources: Solid red circle (this work). Solid blue squares (28). See Eq. S1 in

section 2.8 for the definition of Δ17O.

Compared to the D’Orbigny age anchor, the slope of 53Mn/55Mn = (5.90±0.67) × 10-6 defined

by Sutter's Mill and other carbonaceous chondrites (Fig. S20) translates into an absolute age of

4,566.57±0.66 My. This suggests a nebula-wide, moderately volatile element depletion event has

occurred within ±0.66 My. It constrains the timescale of accretion and compaction of the

carbonaceous chondrite parent bodies, including that of Sutter’s Mill (this work), to within ~ 1

Ma (28) after CAI formation at 4,567.60±0.36 My (90,91). This suggests the first stage of planet

formation from dust to planetesimals is completed within ~1 My (28,86). The nuclear anomaly

of ε54Cr vs. Δ17O plot (Fig. S20) places Sutter's Mill squarely in the CM field (28). 54Cr, together

with few other nuclear anomalies, is becoming a tool on par with Δ17O to classify meteorites

(92).

36

2.8. Oxygen Isotope Analyses

Laser Fluorination

The oxygen isotopic compositions of silicates in SM43 were measured using the laser

fluorination technique of Farquhar and Thiemens (93) at UC San Diego. SM43 was separated

into 1-2mg aliquots, which were laser fluorinated in a single session. Data were normalized to

the NBS-28 quartz standard, samples of which were analyzed immediately before and after the

meteorite analyses. The isotopic compositions of the product O2 were measured on a Finnigan

MAT 253, and average uncertainty in 18O/16O is ± 0.03‰ (1σ) and 17O/16O is ± 0.06‰ (1σ).

Oxygen isotope analyses at UCLA were performed by infrared laser-assisted fluorination

following the general method developed by (94) and modified for triple-oxygen isotope ratio

analysis by (95). Oxygen isotope ratios were measured on oxygen (as O2 gas) extracted from the

meteorite by heating with a 20 Watt CO2 laser in the presence of purified F2 gas. The fluorine

gas was delivered to the samples by heating K2NiF6 . KF powder to a temperature greater than

250 °C. The laser was operated at 5 to 11 W with 10 Hz beam modulation. Liberated O2 was

separated from residual F2 by reaction of the latter over hot KBr and cryogenic trapping of Br2

gas, then trapped onto molecular sieve 13X at -196 °C. Ubiquitous trace amounts of NF3 cause 17O16O interferences (at mass/charge = 33) due to NF produced in the source of the mass

spectrometer. Trace NF3 was removed by distilling the oxygen from the 13X molecular sieve at

-130 °C to a second molecular sieve at -196 °C for 30 minutes. Analyte oxygen was expanded

directly from the second molecular sieve into one side of the dual inlet of the isotope ratio mass

spectrometer by heating to > 110°C for 30 minutes. Simultaneous measurements of 33O2/32O2

and 34O2/32O2 (yielding 17O/16O and 18O/16O, respectively) were made on a ThermoFinnigan

MAT Delta mass spectrometer. Six blocks of 20 cycles, each cycle consisting of an 8 second

integration, comprised each measurement. Quoted uncertainties are 1 standard error (standard

deviation about the mean) for the six blocks.

Oxygen isotope data from both UCSD and UCLA are consistently reported in Table S10 as

δ17O’ and δ18O’ defined as: , where xxO refers to either 17O or 18O, respectively, and δxxO in turn is parts per 1,000 deviations from Standard Mean Ocean

Water (SMOW) as the reference, . The Δ17O

37

values reported are relative to a mass fractionation curve passing through the origin on the

Standard Mean Ocean Water scale with an exponent β which relates the mass fractionation

factors for 17O/16O and 18O/16O according to the relation (96), where α17 =

(17O/16O)Sample/(17O/16O)SMOW, and α18 = (18O/16O)Sample/(18O/16O)SMOW. Thus Δ17O is calculated

consistently and accurately as

(Eq. S1)

which is used to assess the deviation from the empirically defined Terrestrial Fractionation Line

(TFL) as in (97). Δ17O calculated using β = 0.528 (UCLA) and β = 0.5247 (UCSD) are both

shown in Table S10 in two separate columns. The tank O2 used as an internal standard in this

study at UCLA was calibrated against air O2 (δ18OSMOW = 23.5 per mil, Δ17O = -0.35 per mil)

and San Carlos olivine (δ18OSMOW = 5.2 per mil, Δ17O = 0.00 per mil).

Table S10: Oxygen isotopic composition of Sutter’s Mill meteorite: Laser Fluorination using BrF5.

Isotopes relative to SMOW, measured isotopic compositions have been corrected for contribution from

blank in laser fluorination system and have been compared to measured compositions of laser fluorinated

samples of NBS-28 quartz standard (UCSD) and of San Carlos olivine standard (UCLA).

Sample ID δ17O (‰)

±1σ (‰)

δ18O (‰)

±1σ (‰)

Δ17O (‰) β=0.528

Δ17O (‰) β=0.5247

±1σ (‰)

Lab

SM43-2 4.034 0.044 11.351 0.028 -1.960 -1.922 0.029 UCSD SM43-3 3.630 0.073 10.658 0.044 -1.997 -1.962 0.050 UCSD SM43-4 3.643 0.058 10.436 0.013 -1.867 -1.833 0.051 UCSD SM43-6 3.757 0.052 10.763 0.037 -1.926 -1.890 0.033 UCSD SM43-8 4.033 0.053 10.564 0.023 -1.545 -1.510 0.041 UCSD SM51-1 5.898 0.010 16.657 0.011 -2.898 -2.843 0.007 UCLA SM51-2 6.167 0.018 16.824 0.003 -2.716 -2.660 0.018 UCLA

Secondary Ion Mass Spectrometry (SIMS)

Oxygen-isotope compositions of olivines and carbonates were measured in situ with the UH

Cameca ims-1280 SIMS. A ~0.8-1.2 nA Cs+ primary ion beam was focused to a diameter of ~5

µm and rastered over ~10 × 10 µm2 area for presputtering (120 seconds). After presputtering, the

raster size was reduced to 7 × 7 µm2 for automated centering of the secondary ion beam followed

by data collection. An energy window of 40 eV was used. Normal incident electron flood gun

was used for charge compensation with homogeneous electron density over region of ~70 µm in

diameter. Three oxygen isotopes (16O−, 18O−, and 17O−) were measured in multicollection mode

38

using the multicollection Faraday cups L’2 and H1 and the monocollection electron multiplier,

respectively. Mass-resolving power for 17O− and for 16O− and 18O− were set to ~5,500 and

~2,000, respectively. 16OH− signal was monitored in every spot measured for oxygen isotopes

and was typically less than 106 cps, while typical 17O− count rate was 2 × 105 cps. Contribution

of 16OH− onto 17O− was corrected based on a peak/tail ratio measured in same analytical session.

The correction was typically less than 0.1‰ (~0.2‰ at most).

Fig. S21. Oxygen-isotope compositions of calcite, dolomite and olivines in type I and II chondrules,

and amoeboid olivine aggregates from SM51 (this study), and bulk calcite and dolomite from other CM

chondrites, data from (34). TFL: terrestrial fractionation line; CCAM: carbonaceous chondrite anhydrous

mineral line (44); Y&R: Young and Russell line (48).

Instrumental mass fractionation effects for olivine, calcite, and dolomite were corrected by

analyzing San Carlos olivine, UWC-1 calcite, and UW6250 dolomite standards, respectively.

The standards were analyzed repeatedly before and after each run. Reported errors (2σ) include

both the internal measurement precision and the external reproducibility (~0.6-1.2‰ (2SD) in

both δ17O and δ18O) of standard data obtained during a given session. After analysis, the location

of each probe spot was re-imaged to check for beam overlap between phases, and to identify

large cracks or impurities that may have affected the result. Oxygen-isotope compositions of

39

chondrule and AOA olivines (Fig. S21) plot along the carbonaceous chondrite anhydrous

mineral CCAM line; ferroan chondrule olivines (Fa27−46) are 16O-depleted (Δ17O = δ17O −

0.52×δ18O ~ −2.0‰) relative to magnesian (Fa0.5−2) olivines in chondrules (Δ17O ~ −4.0 to

−8.7‰, respectively) and AOAs (Δ17O ~ −23‰). Note that Δ17O = δ17O − 0.52×δ18O is simply

the first-order Taylor expansion of the Eq. S1.

Table S11. Oxygen-isotope compositions of olivines in AOAs, type I and type II chondrules in Sutter's Mill, SM51-1.

mineral   δ18O 2σ δ17O 2σ Δ17O 2σ AOA   -­‐45.6   1.2   -­‐46.8   0.8   -­‐23.1   1.0  AOA   -­‐45.7   1.1   -­‐46.9   0.8   -­‐23.1   1.0  AOA   -­‐45.4   1.2   -­‐47.4   0.8   -­‐23.8   1.0  type  I  chd   -­‐1.6   1.1   -­‐5.2   0.8   -­‐4.4   1.0  type  I  chd   -­‐1.5   1.1   -­‐5.1   0.8   -­‐4.3   1.0  type  I  chd   -­‐2.2   1.1   -­‐5.1   0.8   -­‐4.0   1.0  type  I  chd   3.5   1.1   -­‐0.1   0.7   -­‐1.9   0.9  type  I  chd   -­‐4.1   1.2   -­‐7.4   0.7   -­‐5.3   0.9  type  I  chd   -­‐4.1   1.1   -­‐7.8   0.8   -­‐5.6   1.0  type  I  chd   -­‐5.0   1.1   -­‐7.5   0.7   -­‐4.9   0.9  type  I  chd   -­‐4.8   1.1   -­‐7.5   0.8   -­‐5.1   1.0  type  I  chd   -­‐3.4   1.1   -­‐7.5   0.8   -­‐5.7   1.0  type  I  chd   -­‐9.7   1.2   -­‐13.4   0.8   -­‐8.3   1.0  type  I  chd   -­‐9.5   1.1   -­‐13.1   0.8   -­‐8.2   1.0  type  I  chd   -­‐8.6   1.1   -­‐13.2   0.7   -­‐8.7   1.0  type  I  chd   -­‐9.1   1.1   -­‐13.1   0.8   -­‐8.3   0.9  type  I  chd   -­‐6.1   1.2   -­‐9.8   0.8   -­‐6.6   1.0  type  I  chd   -­‐6.3   1.1   -­‐9.8   0.8   -­‐6.5   1.0  type  I  chd   -­‐6.8   1.1   -­‐10.7   0.8   -­‐7.2   1.0  type  I  chd   -­‐6.7   1.1   -­‐11.4   0.8   -­‐7.9   1.0  type  I  chd   -­‐7.3   1.1   -­‐11.6   0.8   -­‐7.8   1.0  type  I  chd   -­‐5.4   1.2   -­‐8.5   0.8   -­‐5.7   1.0  type  I  chd   -­‐4.8   1.1   -­‐9.3   0.8   -­‐6.8   1.0  type  II  chd   1.7   1.1   -­‐1.1   0.8   -­‐2.0   1.0  type  II  chd   2.4   1.1   -­‐0.7   0.7   -­‐1.9   0.9  type  II  chd   2.7   1.2   -­‐0.7   0.7   -­‐2.2   0.9  type  II  chd   3.5   1.1   -­‐0.1   0.7   -­‐1.9   0.9  

Aqueous alteration resulted in replacement of primary anhydrous minerals by phyllosilicates,

magnetite, Fe,Ni-sulfides, and carbonates – calcite (CaCO3) and dolomite ((Ca,Mg,Mn)CO3)

(Figs. 2b−d, main text). On a three-isotope oxygen diagram (δ17O vs. δ18O), calcites show a large

range of δ18O (+13‰ to +39‰) with Δ17O (= δ17O − 0.52×δ18O) decreasing from −0.3‰ to

40

−3.8‰ with most values near the lower value that is similar to primary silicates (Fig. S21).

Overall the trend is one of highly variable δ18O at a largely invariant Δ17O that encompasses the

range in both parameters exhibited by both CM and CI carbonates (Fig. 4, main text). Such a

trend requires a buffering of the fluid by exchange with rock over a large range of temperatures

(33).

Table S12. Oxygen-isotope compositions of carbonates in Sutter's Mill, SM51-1.

mineral δ18O 2σ δ17O 2σ Δ17O 2σ dolomite 24.8 1.1 9.3 1.1 -3.6 1.2 dolomite 25.2 1.2 9.8 1.1 -3.3 1.2 dolomite 25.1 1.2 9.7 1.1 -3.4 1.3 dolomite 24.1 1.1 9.7 1.1 -2.9 1.2 dolomite 26.1 1.2 10.6 1.1 -3.0 1.2 dolomite 25.5 1.2 9.3 1.1 -4.0 1.3 dolomite 24.3 1.1 9.8 1.1 -2.8 1.3 dolomite 23.5 1.1 8.8 1.1 -3.4 1.2 dolomite 24.2 1.2 9.5 1.1 -3.1 1.2 dolomite 24.6 1.2 9.8 1.1 -3.0 1.2 dolomite 24.1 1.1 9.8 1.1 -2.8 1.2 calcite 32.5 1.4 15.3 0.9 -1.7 1.2 calcite 33.7 1.3 15.8 0.9 -1.7 1.1 calcite 30.5 1.3 14.3 0.9 -1.6 1.1 calcite 31.8 1.2 15.1 0.9 -1.5 1.1 calcite 24.3 1.2 10.4 0.9 -2.2 1.1 calcite 19.7 1.2 7.4 0.9 -2.8 1.1 calcite 32.9 1.2 15.9 0.9 -1.1 1.1 calcite 32.4 1.3 15.0 1.0 -1.8 1.2 calcite 31.8 1.2 14.5 0.9 -2.1 1.1 calcite 34.6 1.2 15.7 0.9 -2.3 1.1 calcite 13.2 1.3 3.5 1.0 -3.3 1.2 calcite 28.8 1.1 13.3 0.9 -1.7 1.0 calcite 30.8 1.6 14.2 1.0 -1.8 1.3 calcite 27.5 1.4 12.2 0.9 -2.1 1.1 calcite 33.0 1.3 15.5 0.9 -1.6 1.1 calcite 33.6 1.2 16.2 1.0 -1.2 1.2 calcite 39.2 1.5 18.8 0.9 -1.6 1.2 calcite 36.9 1.2 18.8 0.9 -0.3 1.1 calcite 33.9 1.3 16.3 0.8 -1.3 1.1 calcite 32.0 1.3 15.4 1.0 -1.2 1.2 calcite 26.5 1.1 11.6 0.8 -2.2 1.0 calcite 15.0 1.2 4.0 0.9 -3.8 1.1

41

Calcites show a large spread of δ18O value (+13‰ to +39‰) with Δ17O = −1.9±1.5‰. A

trend line regressed through the calcite data (Fig. S21), δ17O = 0.62×δ18O − 4.88, is nearly

identical to that reported for CM calcites by Benedix et al. (34), and tracks evolution of fluid

composition from higher to lower Δ17O values with increasing degree of alteration of the CM

parent body.

Dolomites from both lithologies are tightly clustered around δ18O ~ +25‰ with Δ17O =

−3.2±0.7‰ (average ±2 standard deviations), suggesting late-stage precipitation of dolomite

under stringent physico-chemical conditions. Bulk oxygen-isotope composition of SM43 plots in

the field of the extensively aqueously altered CMs, whereas that of SM51 extends the currently

known CM field (Fig. 4, main text), possibly due to higher abundance of δ18O-rich carbonates.

2.9. C, N, and Ar Isotope Analyses

The abundance and isotopic composition of carbon, nitrogen and argon were determined by

stepped combustion-mass spectrometry (Finesse instrument) at the Open University (98,99) in

two separate analytical sessions using 3.565 mg and 6.34 mg chips of whole-rock meteorite from

Fig. S22. Stepwise combustion yield of C content and δ13C for Sutter’s Mill meteorite (SM43),

Murchison (CM), and Maribo (CM). The repeat measurement (right) is also for sample of SM43. The

carbon isotope profile in a duplicate sample (left panel Fig. S22) is well reproduced, though the total δ13C

is lower (6.4 compared to 28.5). This could occur if less carbonate was present in the second aliquot

(Table S14). Carbon release is also a bit different and may indicate a smaller amount of carbonate as well.

42

SM43. The chip was wrapped in platinum foil, then heated under excess oxygen in increments

from room temperature to 1400 °C. Data were corrected for system blank. The results are shown

below in Table S13 and S14.

Table S13. The abundance and isotopic composition of carbon and argon in stepwise combustion.

Temp  °C   C  ppm   δ13C   40Ar  cc   40Ar/36Ar     36Ar  corr  cc/g  200   158.3   -­‐16.3   3.92E-­‐08   253.3   6.12E-­‐09  250   284   -­‐5.6   2.97E-­‐08   198.1   1.38E-­‐08  300   535.4   -­‐7   2.89E-­‐08   124.5   3.77E-­‐08  350   1090.6   1.6   1.44E-­‐08   51.6   6.45E-­‐08  400   2332.8   -­‐1.9   1.17E-­‐08   27.8   1.07E-­‐07  450   3908.4   4.2   8.17E-­‐09   13.2   1.65E-­‐07  500   4281.1   5.9   6.02E-­‐09   8.5   1.93E-­‐07  550   3290.5   37.6   6.21E-­‐09   18.7   8.71E-­‐08  600   4205.9   57   5.24E-­‐09   72.2   1.54E-­‐08  650   3233.4   65.8   5.27E-­‐09   205.1   2.20E-­‐09  700   631   49   4.23E-­‐09   214   1.52E-­‐09  750   390.4   39.1   9.33E-­‐09   222.2   2.91E-­‐09  800   155   46.5   4.42E-­‐09   187.7   2.40E-­‐09  850   100.3   41.2   3.70E-­‐09   260.6   4.64E-­‐10  900   177.6   33.3   4.94E-­‐09   203   2.13E-­‐09  950   268   127.2   3.65E-­‐09   240.4   7.88E-­‐10  

1000   60.9   125.1   3.84E-­‐09   241   8.20E-­‐10  1050   36.2   108.7   3.63E-­‐09   284.7   1.25E-­‐10  1100   20.5   39.6   4.25E-­‐09   249.7   7.33E-­‐10  1150   13.4   5   4.48E-­‐09   291.3   5.45E-­‐11  1200   7.5   -­‐12.1   4.54E-­‐09   256.9   6.40E-­‐10  1250   4.6   -­‐23.3   5.61E-­‐09   231.7   1.46E-­‐09  1300   4.4   -­‐24.8   6.22E-­‐09   248.1   1.12E-­‐09  1350   4.8   -­‐25.8   7.20E-­‐09   275.3   4.91E-­‐10  1400   6.1   -­‐25.8   6.39E-­‐09   288.7   1.33E-­‐10  

    25201.1   28.5           7.07E-­‐07  

43

Table S14. The abundance and isotopic composition of carbon, nitrogen, helium, argon and xenon stepwise combustion. Temp ºC C ppm δ13C 1σ N ppm δ15N 1σ 4He cc/g 36Ar cc/g 132Xe cc/g

200 128.1 -19.5 0.51 4.2 13.5 0.5 4.07E-08 3.71E-09 2.87E-10 250 422.7 -18.1 0.31 11.1 -5.3 0.2 4.32E-07 1.29E-08 2.50E-10 300 664.8 -13.5 0.64 10.6 -1.7 0.2 4.97E-07 3.54E-08 2.37E-11 350 1492.6 -8.7 0.5 18.2 -3.6 0.2 8.20E-07 4.73E-08 7.28E-11 400 2345.1 -5 0.78 34.7 -8 0.2 1.16E-06 7.89E-08 1.75E-10 450 4381.6 -6.1 0.52 136.7 -17.3 0.1 3.26E-06 1.78E-07 3.33E-10 500 4394.4 -6.3 0.44 165.7 -11 0.1 6.59E-06 2.24E-07 2.04E-10 550 3194.3 2.7 0.95 107.3 18 0.1 7.06E-06 1.40E-07 9.50E-11 600 2635.3 40.5 1.13 26.4 42.7 0.2 6.32E-07 3.94E-08 2.61E-11 650 994.8 56.9 0.77 7.7 25.9 0.3 2.28E-07 3.14E-09 3.42E-11 700 435.8 48.6 1.05 8.6 13 0.2 2.12E-07 2.62E-09 4.94E-11 750 377.9 45.2 0.4 10.9 23.6 0.2 8.45E-08 3.85E-09 5.50E-11 800 158.8 54.2 0.44 2.8 14.3 0.6 6.10E-08 1.56E-09 3.49E-12 850 103 30.5 0.32 4.3 38.7 0.4 2.37E-09 4.53E-12 900 125.3 30.1 0.53 6.2 52.2 0.3 3.43E-09 4.37E-12 950 65.5 104.8 0.55 1.6 7.8 1 4.54E-09 8.03E-12

1000 31.8 93 0.48 0.3 3.5 5.1 1050 24 96.7 0.49 0.4 7.2 3.7 1100 18.8 51.1 0.56 0.5 16 3.4 1200 14.9 8.7 0.54 0.3 24.9 4.6 1300 10.6 -25.5 0.45 0.2 37.5 7.2 1400 7.3 -27 0.23 0.3 42.9 4.9

22027 6.4 559.1 -0.6 2.11E-05 7.81E-07 1.63E-09

Fig. S23. Organic nitrogen associated with

carbon is significantly lighter than in Tagish

Lake (and Murchison). The similarity in the

N isotope profiles for the meteorites at high

T can be explained by the light N signature

of SiC.

44

Fig. S24. Sutter’s Mill has the lowest N/C ratio δ15N, compared to other CM meteorites, suggesting

Sutter’s Mill contains different organic nitrogen components.

Fig. S25. Stepwise release pattern of 36Ar for

Sutter’s Mill (SM43), Murchison, and Maribo. All

noble gases are released at the same time with

carbon indicating that their carrier is

carbonaceous.

Almost 95% of the carbon in SM43

combusted below 650ºC; the δ13C increased

with temperature from -16 to +65‰. Carbon

and nitrogen isotopic compositions vary

widely between fragments, with δ13C and

δ15N values ranging between −13‰ and +28.5‰ and between −0.6‰ and +16.7‰, respectively.

2.10. Noble Gases (He, Ne, Ar, Kr and Xe)

Chips weighing 2.346 and 3.169 mg separated from SM43, and 1.638 and 4.029 mg from SM51

were used for noble gas analysis with a modified-MM5400 noble gas mass spectrometer at the

Department of Earth and Planetary Sciences, Kyushu University. The mass spectrometer is

45

equipped with noble gas extraction furnace and noble gas purification line with two Ti-Zr getters

and two charcoal traps. Each sample was wrapped in thin Al-foil and all the samples were

installed in a sample holder attached to the furnace. Whole extraction furnace and purification

line for noble gases were heated at about 250 ºC for a day under ultra-high vacuum condition to

remove atmospheric contamination. During the heating procedure, the meteorite samples were

kept at ca. 130 ºC to remove atmospheric noble gas contamination. Prior to noble gas extraction

from the samples in a Mo-crucible of the extraction furnace, the crucible was degassed at the

temperature of ca. 1900 ºC repeatedly to lower the blank level.

Noble gases were extracted by totally melt the samples, SM43-1 (the 2.346 mg fragment) and

SM51-2 (the 1.638 mg fragment) at 1800 ºC in the Mo-crucible. Remaining two samples, the

3.169 mg fragment of SM43-2 and the 4.029 mg fragment of SM51-1 were heated stepwise at

the temperatures of 600, 900, 1400, and 1800 ºC to extract noble gases of different origins

separately.

Sensitivities and mass discrimination correction factors for noble gases were determined by

measuring a known amount of atmosphere. Mass discrimination for 3He/4He ratio was

determined using a 3He and 4He mixture with 3He/4He = 1.71 × 10-4. Blank levels were 2 × 10-11,

2 × 10-12, 7 × 10-10, 4 × 10-14, and 1 × 10-14 cm3STP for 4He, 20Ne, 40Ar, 84Kr, and 132Xe,

respectively. The blank correction was applied to all the noble gas data. Experimental errors for

isotopic ratios are given in terms 1σ, and the uncertainties for concentration determination are

estimated to be about 10 % of a given value.

The elemental and isotopic compositions of noble gases determined for 4 fragments from the

Sutter's Mill meteorite, SM43 and SM51, are presented in Tables S15 through S17. Elemental

ratios among Ar, Kr, and Xe show that heavy noble gases in this meteorite are dominated by Q-

gas (Fig. S26), which is a main noble gas component trapped in Q-phases in chondrites. The

concentrations are as high as those observed in CM2 chondrites, consistent with the classification

of this meteorite. A datum point for 600 ºC of SM43 sample apart from Q-component indicates

desorption of terrestrial atmospheric contamination (Fig. S26 and Table S15). The terrestrial

contamination is supported by the 40Ar/36Ar ratio of 273 in this fraction, which is close to

atmospheric value of 296. In contrast to the SM43, degree of atmospheric contamination for

SM51 is insignificant (Fig. S26).

46

Fig. S26. Elemental compositions of Ar, Kr, and Xe for SM43 (left) and SM51 (right).

Fig. S27. Ne three isotope plot for SM43 (left) and SM51 (right).

The 3He/4He ratios (Table S15) are as low as (1.6-1.9) × 10-4, which are similar to or slightly

higher than those of primitive trapped components, Q (1.23 × 10-4), P3 (≤1.35 × 10-4), and HL

(≤1.7 × 10-4), but distinctly lower than the present-day solar wind value (4.64 × 10-4). Hence, it is

difficult to estimate concentrations of cosmic-ray produced 3He for this meteorite, because in

most cases 3He/4He ratios are much higher than the solar value by production of cosmogenic He

isotopes with 3He/4He ratio of ~0.2. The U, Th-He age is also difficult to estimate because of

abundant primordial He as shown by the 3He/4He ratios and elemental compositions.

47

Table S15. Noble gas concentrations and isotopic ratios of He, Ne, and Ar of Sutter’s Mill SM43 and

SM51. Concentrations are in the unit of 10-9 cm3-STP/g.

SM43-2 4He 3He/4He 22Ne 20Ne/22Ne 21Ne/22Ne 0.000157 9.13 0.0354

600 °C 603 ± 0.000011

1.01 ± 0.26 ± 0.0042

0.000158 8.138 0.0327 900 °C 21600

± 0.000009 12.0

± 0.049 ± 0.0014 0.000185 6.421 0.0224

1400 °C 4830 ± 0.000059

6.34 ± 0.054 ± 0.0017

0.00061 9.2 0.053 1800 °C 6.80

± 0.00036 0.0301

± 5.0 ± 0.047 Total 27040 0.000163 19.4 7.630 0.0295

SM43-1 4He 3He/4He 22Ne 20Ne/22Ne 21Ne/22Ne

0.0001855 7.487 0.02921 1800 °C 28200

± 0.0000072 20.6

± 0.077 ± 0.00094

SM51-1 4He 3He/4He 22Ne 20Ne/22Ne 21Ne/22Ne 0.000269 11.57 0.0384

600 °C 446 ± 0.000020

1.85 ± 0.17 ± 0.0026

0.0001949 8.754 0.03347 900 °C 28600

± 0.0000084 15.5

± 0.033 ± 0.00093 0.000187 8.486 0.0300

1400 °C 7450 ± 0.000015

12.2 ± 0.063 ± 0.0012

0.00038 10.72 0.0523 1800 °C 7.92

± 0.00040 0.474

± 0.37 ± 0.0086 Total 36504 0.000194 30.0 8.85 0.0326

SM51-2 4He 3He/4He 22Ne 20Ne/22Ne 21Ne/22Ne

0.000175 8.628 0.0329 1800 °C 32600

± 0.000014 24.6

± 0.061 ± 0.0011

Neon isotopic ratios (Fig. S27) show interesting features for two different specimens. The

main component of Ne in the SM43 sample is HL or P3, and a small amount of Ne-E(H) is

observed in 1400 ºC fraction (Fig. S27). The carrier phases of the HL and P3 components are

presolar diamonds, while Ne-E(H) is known to be trapped in presolar SiC grains. In the case of

the SM51, on the other hand, Ne in 900 and 1400 ºC fractions plots close to HL and P3, but the

48

datum point of 600 ºC fraction plots in a region related with noble gas component of solar origin

(Fig. S27). No indication of Ne-E(H) in this sample was observed. The presence of Ne

component related to solar Ne might have resulted from an implantation of solar gases to surface

materials of the parent asteroid (26).

Table S15 (cont.).

SM43-2 36Ar 38Ar/36Ar 40Ar/36Ar 84Kr 132Xe 0.1899 272.6

600 °C 44.4 ± 0.0030 ± 4.1

1.59 0.617

0.1862 24.04 900 °C 197

± 0.0015 ± 0.50 2.55 2.04

0.1866 2.98 1400 °C 442

± 0.0015 ± 0.17 5.11 6.38

0.1835 6.6 1800 °C 12.0

± 0.0040 ± 5.9

0.147 0.261

Total 695 0.1866 26.23 9.4 9.3

Sm43-1 36Ar 38Ar/36Ar 40Ar/36Ar 84Kr 132Xe 0.1880 27.78

1800 °C 705 ± 0.0014 ± 0.34

10.0 10.1

SM51-1 36Ar 38Ar/36Ar 40Ar/36Ar 84Kr 132Xe 0.1870 163.7

600 °C 25.9 ± 0.0026 ± 2.9

0.481 0.380

0.1870 10.41 900 °C 190

± 0.0016 ± 0.38 1.96 1.94

0.1867 1.43 1400 °C 512

± 0.0013 ± 0.11 5.65 7.51

0.1887 5.4 1800 °C 13.9

± 0.0029 ± 4.0

0.155 0.252

Total 742 0.1868 9.47 8.25 10.1

SM51-2 36Ar 38Ar/36Ar 40Ar/36Ar 84Kr 132Xe 0.1856 13.30

1800 °C 656 ± 0.0013 ± 0.29

8.03 9.57

49

Table S16: Isotope ratios of Kr in the Sutter’s Mill CM chondrite. Concentrations are in the unit of 10-9

cm3-STP/g.

SM43-2 84Kr 78Kr/84Kr 80Kr/84Kr 82Kr/84Kr 83Kr/84Kr 86Kr/84Kr 0.00629 0.03770 0.1923 0.1948 0.3062 600 °C 1.59

± 0.00057 ± 0.00108 ± 0.0028 ± 0.0041 ± 0.0059

0.00561 0.03886 0.1938 0.1996 0.3130 900 °C 2.55 ± 0.00050 ± 0.00131 ± 0.0029 ± 0.0040 ± 0.0048

0.00588 0.03765 0.1948 0.2006 0.3098 1400 °C 5.11 ± 0.00013 ± 0.00094 ± 0.0037 ± 0.0029 ± 0.0044

0.0063 0.0408 0.198 0.199 0.320 1800 °C 0.15 ± 0.0014 ± 0.0047 ± 0.011 ± 0.013 ± 0.014 Total 9.40 0.00588 0.0380 0.1942 0.1993 0.3102

SM43-1 84Kr 78Kr/84Kr 80Kr/84Kr 82Kr/84Kr 83Kr/84Kr 86Kr/84Kr

0.00593 0.03927 0.1985 0.2030 0.3127 1800 °C 10.0 ± 0.00023 ± 0.00064 ± 0.0022 ± 0.0030 ± 0.0023

SM 51-1 84Kr 78Kr/84Kr 80Kr/84Kr 82Kr/84Kr 83Kr/84Kr 86Kr/84Kr

0.00618 0.04029 0.1899 0.1961 0.3083 600 °C 0.481 ± 0.00081 ± 0.00475 ± 0.0063 ± 0.0058 ± 0.0099

0.00608 0.03882 0.1909 0.1970 0.3100 900 °C 1.96 ± 0.00042 ± 0.00088 ± 0.0044 ± 0.0032 ± 0.0065

0.00597 0.03841 0.1971 0.2001 0.3081 1400 °C 5.65 ± 0.00028 ± 0.00101 ± 0.0032 ± 0.0018 ± 0.0026

0.0066 0.0405 0.202 0.202 0.308 1800 °C

0.155 ± 0.0014 ± 0.0046 ± 0.011 ± 0.012 ± 0.013 Total 8.2 0.00602 0.0387 0.1953 0.1991 0.3085

SM 51-2 84Kr 78Kr/84Kr 80Kr/84Kr 82Kr/84Kr 83Kr/84Kr 86Kr/84Kr

0.00607 0.03883 0.1910 0.1958 0.3067 1800 °C 8.03 ± 0.00038 ± 0.00146 ± 0.0043 ± 0.0044 ± 0.0042

50

Table S17. Isotopic ratios of Xe in the Sutter’s Mill CM Chondrite. Concentrations are in the unit of 10-9

cm3-STP/g.

SM 43-2 132Xe 124Xe/132Xe 126Xe/132Xe 128Xe/132Xe 129Xe/132Xe 0.00350 0.00329 0.0753 1.080 600 °C

0.617 ± 0.00017 ± 0.00024 ± 0.0022 ± 0.013 0.00440 0.00383 0.0813 1.066 900 °C 2.04 ± 0.00028 ± 0.00013 ± 0.0013 ± 0.008 0.004243 0.00396 0.0813 1.0461 1400 °C 6.38 ± 0.000076 ± 0.00011 ± 0.0010 ± 0.0030 0.00407 0.00405 0.0847 1.066 1800 °C

0.261 ± 0.00033 ± 0.00057 ± 0.0029 ± 0.024 Total 9.30 0.00422 0.00389 0.0810 1.053

SM 43-1 132Xe 124Xe/132Xe 126Xe/132Xe 128Xe/132Xe 129Xe/132Xe

0.00415 0.003835 0.07945 1.0460 1800 °C 10.1 ± 0.00019 ± 0.000057 ± 0.00079 ± 0.0014

SM 51-1 132Xe 124Xe/132Xe 126Xe/132Xe 128Xe/132Xe 129Xe/132Xe

0.00407 0.00345 0.0760 1.036 600 °C 0.380 ± 0.00053 ± 0.00027 ± 0.0029 ± 0.012

0.00439 0.00400 0.0810 1.064 900 °C 1.94 ± 0.00026 ± 0.00027 ± 0.0009 ± 0.006 0.00423 0.00393 0.0804 1.048 1400 °C 7.51 ± 0.00019 ± 0.00008 ± 0.0007 ± 0.004 0.00445 0.00397 0.0818 1.048 1800 °C

0.252 ± 0.00076 ± 0.00071 ± 0.0019 ± 0.013 Total 10.1 0.00426 0.00393 0.0804 1.051

SM 51-2 132Xe 124Xe/132Xe 126Xe/132Xe 128Xe/132Xe 129Xe/132Xe

0.00423 0.00387 0.0798 1.041 1800 °C 9.57 ± 0.00013 ± 0.00016 ± 0.0006 ± 0.004

Cosmogenic 21Ne concentrations are very low and not easy to estimate for this meteorite. We

assume that Ne isotopic ratios initially trapped in the meteorite were those plotted on mixing

lines; one is connecting Solar-Ne and P3-Ne and another P3-Ne and Ne-E, then isotopic ratios of

trapped Ne for each fraction can be calculate as the coordinates of the intersection between the

mixing line and a line connecting cosmogenic Ne and measured isotopic ratios for each fraction

as shown in Fig. S27. Concentrations of cosmogenic 21Ne and cosmic-ray exposure ages

obtained for each fraction are summarized in Table S18. An average exposure age of 0.051 ±

0.006 My is obtained for this meteorite using a production rate of 2 × 10-9 cm3-STP/g/My (14).

The production rate is proposed for an object smaller than ~10 cm in radius or near surface of

51

larger object. The production rate increases up to ~50% in large object (R > ca. 25 cm). The

short exposure age is an important characteristic of the Sutter's Mill meteorite.

Table S17 (cont.).

SM 43-2 132Xe 130Xe/132Xe 131Xe/132Xe 134Xe/132Xe 136Xe/132Xe 0.1551 0.811 0.387 0.3252 600 °C

0.617 ± 0.0045 ± 0.011 ± 0.011 ± 0.0085 0.1612 0.8280 0.3915 0.3359 900 °C 2.04 ± 0.0026 ± 0.0063 ± 0.0019 ± 0.0047 0.1628 0.8226 0.3812 0.3172 1400 °C 6.38 ± 0.0016 ± 0.0043 ± 0.0033 ± 0.0024 0.1654 0.833 0.387 0.3225 1800 °C

0.261 ± 0.0040 ± 0.017 ± 0.010 ± 0.0059 Total 9.30 0.1620 0.8233 0.3840 0.3220

SM 43-1 132Xe 130Xe/132Xe 131Xe/132Xe 134Xe/132Xe 136Xe/132Xe

0.16126 0.8188 0.3859 0.3164 1800 °C 10.1 ± 0.00088 ± 0.0053 ± 0.0024 ± 0.0017

SM 51-1 132Xe 130Xe/132Xe 131Xe/132Xe 134Xe/132Xe 136Xe/132Xe

0.1610 0.8111 0.3827 0.3149 600 °C 0.380 ± 0.0035 ± 0.0151 ± 0.0040 ± 0.0050

0.1609 0.8175 0.3923 0.3344 900 °C 1.94 ± 0.0029 ± 0.0078 ± 0.0036 ± 0.0042 0.1630 0.8249 0.3824 0.3186 1400 °C 7.51 ± 0.0008 ± 0.0032 ± 0.0011 ± 0.0012 0.1628 0.8211 0.3791 0.3149 1800 °C

0.252 ± 0.0036 ± 0.0087 ± 0.0075 ± 0.0060 Total 10.1 0.1625 0.8228 0.3842 0.3214

SM 51-2 132Xe 130Xe/132Xe 131Xe/132Xe 134Xe/132Xe 136Xe/132Xe

0.1618 0.8243 0.3845 0.3231 1800 °C 9.57 ± 0.0014 ± 0.0036 ± 0.0030 ± 0.0026

Argon isotopic ratios also show that Ar in these samples are mostly primitive trapped

components as indicated by 38Ar/36Ar ratios of ca. 0.188 and low 40Ar/36Ar ratios less than 25

except for 600 ºC fractions, to which atmospheric contamination is observed (Table S15).

Isotopic ratios of Kr and Xe (Table S16 and S17) are almost identical with those of Q-Kr and

Xe. Isotopic ratios of Xe in 600 ºC fractions are affected by terrestrial atmospheric Xe. A small

excess in 136Xe in 900 ºC fractions indicates a presence of HL-Xe component trapped in presolar

diamonds.

52

The 40Ar/36Ar ratios for the meteorite samples are higher than the primitive value of 10-4.

The increase in 40Ar/36Ar ratios was caused by in-situ produced 40Ar from 40K in the meteorite,

or addition of contaminating terrestrial atmospheric Ar with high value of 296 after fall to the

earth. Upper limit of K-Ar age for these samples can be estimated using the total 40Ar

concentrations and K concentrations. For the measured K concentration of 363 ppm (Table S7),

K-Ar ages become as young as 2.4-3.9 Gy, while ca. 4.5 Gy is obtained when the abundance of

K is100-200 ppm K in the sample studied here. The calculation suggests a low K concentration

for this particular sample, or the K-Ar system is disturbed due to a recent heating event(s).

Table S18. Overview of Cosmic Ray Exposure Age measurements for noble gases.

Sample Temp.

°C 21Ne-cosm

10-9 cm3-STP/g ± T21 My

± My

SM43-2 600 0.0065 0.0044 900 0.0747 0.0173 1400 0.0092 0.0113 1800 0.0007 0.0028 Total 0.0912 0.0213 0.046 0.011

SM43-1 1800 0.0991 0.0200 0.050 0.010

SM51-1 600 0.0138 0.0050 900 0.0731 0.0149 1400 0.0163 0.0145 1800 0.0106 0.0048 Total 0.1139 0.0220 0.057 0.011

SM51-2 1800 0.1039 0.0285 0.052 0.014 Average 0.051 0.006

2.11. X-ray Tomography

SM3, 9, 18, 51, and 54 were shipped to AMNH in Al foil in Ziploc bags, handled with latex

gloves, and mounted in cylinders of Scotch transparent tape. X-ray computed tomography (CT)

scanning (20) was performed on the entirety of each stone (Table S19) on the GE Phoenix

VtomexS scanner at AMNH, at 1000 ms exposure, with voltages 110-130 kV, and currents 120-

150 nA, in horizontal and vertical tiles, usually with a 0.1mm Cu beam filter Reconstructed

density maps were output as stacks of TIF format files with 16-bit values describing the x-ray

53

attenuation of each cubic volume element (voxel) in the field of view. Volumes were computed

from scans using ImageJ and Volume Graphics software.

Table S19. CT imaging studies. Sample mass, CT resolution (µm per voxel edge), number of image

stacks, measured volume (mm3), and computed density (g/cm3) are listed.

Scan label Mass (g) Resolution (µm/vxl)

Tiles Volume (mm3)

Density (g/cm3)

Lab

SM3_22A 4.950 22.189 1 2200.0 2.250 AMNH SM9_24A 6.235 24.543 1 2685.7 2.322 AMNH SM18_14A 5.317 13.975 4 2466.5 2.156 AMNH SM51_30A 8.990 30.765 1 3860.2 2.329 AMNH SM51_14A 8.990 14.348 6 4004.6 2.245 AMNH SM51* 8.990 16.670 1 3812.0 2.358 UCD SM54_12B 4.140 12.175 4 1855.1 2.232 AMNH SM73* 8.170 22.57 1 3452.0 2.367 UCD

SM 51 and SM73 were also imaged at the Center for Molecular and Genomic Imaging at

UC Davis. X-ray tomographic images were obtained with a MicroXCT-200 specimen CT

scanner (Xradia Inc.). The CT scanner has a variable x-ray source capable of a voltage range of

20-90kV with 1-8W of power. The samples were secured in place using custom-built holders

such that the samples did not come in contact with any adhesive material. Samples were mounted

on the scanners sample stage, which has submicron level of position adjustments. Scan

parameters were adjusted as needed. First the source and detector distances were adjusted based

on sample size and the optimal field of view for the given region of interest. Once the source and

detector settings were established, the optimal x-ray filtration was determined for selecting

among one of 12 filters. Following this procedure, the optimal voltage and power settings were

determined. Series of images were reconstructed varying the center shift and beam hardening

parameters to obtain optimized images. Images were reconstructed into 16-bit values.

Samples SM3 and SM9 appear to contain a dominant lithology characterized by abundant

200 to 400 µm diameter clasts (chondrules or CAIs), and 0.05 - 0.15 µm metal oxide or sulfide

grains. A second lithology, with higher average atomic mass (Z) matrix and more abundant

clasts, appears as irregular, angular lithic fragments many mm in size. At least one metal grain

~250 µm across, was observed, surrounded by a halo ~750 µm wide, of oxidized or sulfidized

metal. It is unlikely that such a grain would be sampled by random cutting. Several clasts larger

54

than 1 mm include a low-Z spherical object that appears to be concentrically zoned, and a similar

object with zoned high-Z (metal) and low-Z (silicate) layers. Other large clasts are irregular,

blocky objects. While the samples are fractured, and metal grains appear to be altered, no high-Z

veins (e.g., FeO-rich) are observed.

Fig. S28. Fractures surround multiple clasts in SM18 (slice SM18_14A_Z_s1_165, image contrast

enhanced). Six clasts are outlined as recognized by scrolling through the slices above and below this slice.

Contrasts in average atomic mass (brighter is heavier) and texture are evident. Note that fractures in ‘C’

do not extend beyond clast boundaries; fractures in ‘B’ extend from low-Z spherical objects, probably

chondrules; some lithic fragments appear to contain chondrules, while others do not.

The meteorites studied so far exhibit a dominant, primary lithology that is the host for

multiple types of exotic lithic clasts (Fig. S28). With more samples examined with CT, a more

clear description may emerge. The image shown here is 8-bit, with severely compromised

dynamic range due to file size constraint. Further X-ray tomography data are available from the

American Museum of Natural History at http://dx.doi.org/10.5531/sd.eps.1 as well as from UC

Davis at http://www.youtube.com/user/YinLabatUCDavis and

at http://www.youtube.com/user/spelunkerucd/videos .

55

2.12. Neutron Tomography

Neutron imaging is a nondestructive technique that is complementary to X-ray imaging. Unlike

X-rays, neutrons do not interact (or negligibly so at most) with electrons. The interaction cross-

section for X-rays monotonically increases with the number of electrons, i.e. with atomic number

(Fig. S29). For neutrons, however, no direct correlation between neutron cross-section and

atomic number exists. Neutrons directly probe nuclei, giving strong contrast for some elements

that are close to one another in the periodic table, and are even able to distinguish between

different isotopes. Several light elements (notably hydrogen) attenuate neutrons strongly, while

even thick layers of many metals can be penetrated; lead, for example, is used for shielding X-

rays, but is almost transparent for neutrons.

Fig. S29. Mass attenuation coefficient as a function

of atomic number, adapted from (100).

Traditional neutron radiography provides

information on the total attenuation integrated

over the path of the neutrons through the

material. The actual distribution of materials

across that path cannot be extracted in detail.

Neutron computed tomography (NCT) is based

on radiography but provides a three-

dimensional picture of the sample including the

actual distribution of materials throughout the whole sample.

The tomography data was obtained at the University of California, Davis McClellan Nuclear

Research Center (MNRC). The sample was mounted on a turntable where it was exposed to

neutrons. The tomography system utilizes a Li6F-ZnS-Cu scintillation screen to convert the

neutrons into visible light. The green light produced by the scintillator is focused onto a 4

Megapixel CCD camera. In order to obtain the tomography data, 190 radiographs were taken

after every 1° rotation. The exposure time was 45 s for each radiograph at a neutron fluence of

5×106 n/cm2s. The radiographs are corrected for dark current and the flat field before

56

reconstruction using the Imgrec software package developed at Lawrence Livermore National

Laboratory. The resulting voxel size was 116.3 µm. More details can be found in (101,102).

Fig. S30. Reconstructed neutron tomography images of SM54, left: horizontal cut (slice 250), right:

vertical cut (slice 293).

Figure S30 (left, slice 250) shows a reconstructed horizontal cut through the SM54 specimen,

with two broken parts seen as well as the aluminum cup that served as sample holder. Figure S30

(right, slice 293) is a reconstructed image showing a vertical cut through the larger of the two

parts, the ring around the sample is the aluminum wall of the sample holder. In both images dark

inclusions can be seen, these inclusions are quite transparent to neutrons and could be rich in

iron, calcium, aluminum or other elements with low neutron cross-sections. The light inclusions

that can be seen on the lower left part of Fig. S30 (left) and in the right of Fig. S30 (right) are

rich in elements that highly absorbent to neutrons such as hydrogen and carbon. Neutron

tomography results are available for download from the UC Davis website

http://mnrc.ucdavis.edu/data/SuttersMill/index.html as well as for viewing on the YouTube site

at http://www.youtube.com/user/YinLabatUCDavis .

2.13. Cosmogenic Radionuclides

The concentrations of short-lived cosmogenic radionuclides, as well as long-lived

cosmogenic 26Al and natural radioactivity, were measured using non-destructive gamma-ray

spectroscopy. One fragment of Sutter's Mill (SM36) was measured in the ultra low background

counting facility STELLA (SubTerranean Low Level Assay) in the underground laboratories at

57

the Laboratori Nazionali del Gran Sasso (LNGS) in Italy, using a high-purity germanium (HPGe)

detectors of 414 cm3 (103). The specimen was measured at the LNGS only 32 days after the fall,

so that also very short-lived radionuclides such as 48V (half life = 16 d) and 51Cr (27.7d) could

still be detected. The counting time was about two weeks. The counting efficiencies were

calculated using a Monte Carlo code. This code is validated through measurements and analyses

of samples of well-known radionuclide activities and geometries. The uncertainties in the

radionuclide activities are dominated by the uncertainty in the counting efficiency, which is

conservatively estimated at 10%. Tables 20a and 20b summarize the cosmogenic radionuclide

concentrations and the content of natural radioactivity in the sample.

Table S20a. Massic activity (corrected to the time of fall) of cosmogenic radionuclides (in dpm kg-1) in

the 22.3 g specimen SM36 of the Sutter's Mill SM36 meteorite measured by non-destructive gamma-ray

spectroscopy (103). Errors include a 1 sigma uncertainty of ~10% in the detector efficiency calibration.

Nuclide Half-life Energy (keV)

Massic activity (dpm/kg)

48V 16.0 d 983.5/1311.6 17 ± 6 51Cr 27.7 d 320.07 82 ± 24 59Fe 44.5 d 1099/1291 6 ± 3 7Be 53.1 d 477.6 243 ± 29 58Co 70.9 d 810.8 24 ± 3 56Co 77.3 d 846.8/1238/2599 11 ± 2 46Sc 83.8 d 889.3/1120 12 ± 2 57Co 271.8 d 122.1/136 22 ± 2 54Mn 312.3 d 834.8 189 ± 19 22Na 2.60 y 1274.5/1785 122 ± 11 60Co 5.27 y 1173.2/1332.5/2506 34.1 ± 2.7 26Al 7.05x105 y 1808.7/2319 3.8 ± 0.8

Table S20b. Concentrations of primordial radionuclides in the 22.3 g specimen of the Sutter's Mill

meteorite SM36 measured by nondestructive gamma-ray spectroscopy. Errors include a 1σ uncertainty of

~10% in the detector efficiency calibration.

Nuclide Energy (keV) Concentrations U 242/295/352/609/1764/2204 15 ± 2 ng g-1 Th 238/338/583/727/911/968/2614.5 40 ± 6 ng g-1 K 1460.8 594 ± 62 µg g-1

58

2.14. Ultra-high Resolution Mass Spectroscopy and Nuclear Magnetic Resonance Spectroscopy

Flow injection negative electrospray [ESI(-)] ultra high resolution 12 T FTICR mass

spectrometry (36) was performed on 25 mg samples of SM2 and SM12, following extraction

with LC/MS grade methanol (Fig. S31). Thousands of mass signals with good coverage of

isotopologues could be converted into a few hundreds of C, H, O, N, S, P, Na bearing

compositions, indicating less compositional and structural diversity than found in other

carbonaceous chondrites, among which are several fresh carbonaceous chondrites such as CM2

Murchison (36), CM2 Maribo (9) and other carbonaceous chondrite types such as CV, CK, CO,

CI and C-ungrouped.

Fig. S31. FTICR/MS detail on nominal mass 319 of Sutter´s Mill samples SM2 and SM12 compared with

CM2 Murchison and the methanol blank.

While Murchison methanolic extract shows more than hundred m/z signals and elemental

compositions in the mass range 319.0 to 319.4 alone, SM2 and SM12 only show few signals

corresponding to C, H, O, S type of molecules. SM2 and SM12 specifically exhibit many signals

318.8 318.9 319.0 319.1 319.2 319.3m/z

solvent blank

SN 12

Murchison

SN 2

poly S domain

[C17H35O3S]-

[C20H31O3]-

[C18H23O5]-

[C15H11O6S]-

[C9H3O7S3]-

59

in the mass range 318.75 to 319.0 corresponding to oxygen rich and multiple sulphur containing

compounds (poly-S domain). The characteristics found in nominal mass 319 as depicted here are

repeated all over the mass spectra.

Fig. S32. 800 MHz 1H NMR spectra of Sutter´s Mill methanolic extract. (A) one dimensional NMR

spectrum, with vertical expansions (dark blue); red numbers: 1H NMR section integrals. 1H, 1H TOCSY

NMR spectra (mixing time: 70 ms) of (B) unsaturated and (C) saturated chemical environments with

major connectivities indicated: C-CH-CH-C (orange), C-CH-CH-O (green), O-CH-CH-O (blue).

800 MHz 1H NMR spectroscopy of methanolic SM12 Sutter´s Mill extract provided the

highest proportion of branched aliphatics of any of the 20+ meteorites investigated so far using

the same experimental procedure (Fig. S32). Polymethylene contributed for about ten percent to

the purely aliphatic NMR resonances at δH < 1.9 ppm. The ratio of hydrogen bound to sp2

(unsaturated) and those bound to sp3 carbons (saturated) was about 1:50; the OCH to CCH ratio

was close to 1:8. Unsaturated protons fell in the δH range of 6.5 - 9 ppm, indicating the presence

of olefins, oxygenated and carboxylated aromatics, nitrogen heterocycles and PAHs. Typical 1H, 1H spin systems encompassed C3-5 units. OCH-groups with δH: 3.3 - 4.5 ppm were bound to

1.01.52.02.53.03.54.04.55.05.5 ppm

1.0

1.5

2.0

2.5

3.0

3.5

4.0

4.5

5.0

5.5

1.52.02.53.03.54.04.55.05.56.06.57.07.58.08.5 ppm

1.00 0.165.46

39.77

6.46.66.87.07.27.47.67.88.08.28.48.6 ppm

6.4

6.6

6.8

7.0

7.2

7.4

7.6

7.8

8.0

8.2

8.4

8.6

A

B C

60

aliphatic units rather than to other oxygenated aliphatics. In TOCSY NMR spectra, C-HC-CH-O

units were commonly connected to intra aliphatic linkages (C-HC-CH-C) which were prevalent,

whereas the ratio of C-HC-CH-O / O-HC-CH-O units was close to 12:1.

2.15. Raman Spectroscopy

Individual measurements of matrix macromolecular carbon (MMC) in Sutter’s Mill SM12 and

SM2 at the Carnegie Institution of Washington are plotted as a function of Raman G-band center

and width in Fig. S33. The G band position is a function of mean crystallite size within the

MMC, and the full width at half maximum (FWHM) is a function of the distribution of

crystallite sizes within the material. When plotted together, these features define a thermal

metamorphism trend proceeding with poorly crystalline, lightly heated material at upper right to

polycrystalline, relatively annealed material at lower right.

The fragment of SM12 examined here (blue squares) shows evidence of heating to an

intermediate degree between CO3 and CV3 chondrites. CM2 (green diamonds) has not

experienced the same degree of annealing, but has been heated in excess of other CM2

chondrites. Error bars represent peak fitting uncertainties for each individual Raman spectrum.

Fig. S33. Raman G-band center and Full Width at Half Maximum (FWHM).

61

2.16. Liquid Chromatography Mass Spectrometry

Amino acid measurements of a 240 mg chip of SM2 were made at the NASA Goddard Space

Flight Center. The single SM2 chip was powdered in a ceramic mortar and pestle and a 146 mg

aliquot was sealed in a test tube with 1 ml of Millipore Milli-Q Integral 10 (18.2 MΩ, < 1 ppb

total organic carbon) ultrapure water and heated at 100°C for 24 h.

After heating, one half of the water extract was transferred to a separate glass tube, dried

under vacuum, and the residue subjected to a 6 M HCl acid vapor hydrolysis procedure at 150°C

for 3 h to determine total hydrolyzable amino acid content. The acid-hydrolyzed water extracts

were desalted using cation-exchange resin (AG50W-X8, 100-200 mesh, hydrogen form, BIO-

RAD), and the amino acids recovered by elution with 2 M NH4OH (prepared from Millipore

water and NH3(g) (AirProducts, in vacuo). The remaining half of each water extract (non-

hydrolyzed fraction) was taken through the identical desalting procedure in parallel with the

acid-hydrolyzed extracts to determine the free amino acid abundances in the meteorites. The

amino acids in the NH4OH eluates were dried under vacuum to remove excess ammonia; the

residues were then re-dissolved in 100 µL of Millipore water, transferred to sterile

microcentrifuge tubes, and stored at -20°C prior to analysis. Based on our analysis of amino acid

standards taken through the entire extraction and acid hydrolysis procedure, we found no

evidence of significant decomposition, racemization, or thermal degradation of the amino acids

during extraction or acid hydrolysis.

The amino acids in the NH4OH eluates were derivatized with OPA/NAC for 15 minutes at

room temperature. The abundance, distribution, and enantiomeric compositions of the two- to

six-carbon aliphatic amino acids found in SM2 were then measured by ultra performance liquid

chromatography fluorescence detection and time of flight mass spectrometry coupled with o-

phthaldialdehyde/N-acetyl-L-cysteine (OPA/NAC) derivatization. The amino acids and their

enantiomeric ratios were quantified from the peak areas generated from both fluorescence

detection and from the mass chromatogram of their OPA/NAC derivatives. A more detailed

description of the analytical technique and quantification methods used is described elsewhere

(39). The reported amino acid abundances in SM2 below are the average value of three separate

LC-FD/TOF-MS measurements (Table S22). The errors given are based on the standard

deviation of the average value of three separate measurements.

62

Table S21. Summary of the amino acid abundances in parts-per-billion (ppb) in the free (non-hydrolyzed)

and total (6M HCl- hydrolyzed) hot-water extracts of the Sutter's Mill (SM2) carbonaceous chondritea.

Amino Acid Free

(ppb) Total (ppb)

Amino Acid Free (ppb)

Total (ppb)

D-aspartic acid 13 ± 10 26 ± 5 L-aspartic acid 16 ± 1 59 ± 5 D-glutamic acid < 2 29 ± 8 L-glutamic acid 4 ± 2 112 ± 3 D-serine < 3 5 ± 1 L-serine < 3 111 ± 12 glycine 72 ± 14 170 ± 20 D-threonine < 4 < 8 L-threonine < 4 < 8 β-alanine 19 ± 11 45 ± 16 γ-amino-n-butyric acid 3 ± 1 6 ± 3 D-alanine < 2 19 ± 16 L-alanine < 2 35 ± 7 D-β-amino-n-butyric acid < 2 < 5 L-β-amino-n-

butyric acid < 2 < 5

α-aminoisobutyric acid < 2 < 5 D-β-aminoisobutyric acid < 2 2** L-β-

aminoisobutyric acid

< 2 2**

D-α-amino-n-butyric acid* < 2 < 3 L-α-amino-n-butyric acid*

< 2 < 3

D-isovaline < 3 < 8 L-isovaline < 3 < 8 ε-amino-n-caproic acid*** 2 ± 1 87 ± 23 D-valine < 4 < 13 L-valine < 4 37 ± 11

Notes: aExtracts were analyzed by OPA/NAC derivatization and UPLC separation with UV fluorescence

detection and TOF-MS detection at NASA Goddard Space Flight Center. The uncertainties are based on

the standard deviation of the average value of three separate measurements. *Enantiomers could not be

separated under the chromatographic conditions; **Tentative identification; ***Not detected by Arizona

State University team at equal or higher than 10 ppb.

A similar sized sample of the Murchison had a complex distribution of amino acids with a

total C2 to C5 amino acid abundance of ~14,000 parts-per-billion (ppb) (39). SM2, however, was

confirmed to be highly depleted in amino acids and contained trace abundances ranging from ~5

to 170 ppb of glycine, β-alanine, γ-amino-n-butyric acid (γ-ABA), and ε-amino-n-caproic acid

(EACA). Trace amounts of predominately the L-enantiomers of the protein amino acids aspartic

and glutamic acids, alanine, serine, and valine were detected above procedural blank levels and

indicate that SM2 experienced some terrestrial amino acid contamination after its fall to Earth.

Since glycine, β-alanine, γ-ABA, and EACA are all achiral, compound specific carbon isotope

63

Table S22. Carbon and nitrogen composition and isotopic values from bulk elemental analysis-isotope

ratio mass spectrometry. Sample SM2 has the lowest δ13C and the highest δ15N values.

Sample Wt% C N (ppm) δ13C (VPDB) δ15N (AIR)

SM2 1.32 ± 0.03 397 ± 7 -13 ± 1 +16.7 ± 0.3

SM12 1.56 ± 0.01 404 ± 29 2 ± 3 -0.2 ± 0.6

SM51 1.62 ± 0.04 405 ± 8 -3 ± 1 +6.2 ± 0.4

measurements will be necessary to establish the origin of these amino acids in SM2. Other non-

protein amino acids that are rare on Earth, yet commonly found in other CM meteorites such as

α-aminoisobutyric acid (α-AIB) and isovaline, were not identified in SM2 above ppb levels.

However, both D- and L-β-AIB (~2 ppb total) were detected in SM2 and could be extraterrestrial

in origin.

Bulk carbon and nitrogen abundance and isotopic data of samples SM2, SM12, and SM51

were measured at GSFC and are shown in Table S21. Measurements were acquired using a

Costech ECS 4010 combustion elemental analyzer (EA) connected through a Thermo Conflo III

interface to a Thermo MAT 253 isotope ratio mass spectrometer (IRMS). Three separate aliquots

of each powdered sample (~7 to ~16 mg) were weighed in separate tin cups, folded into small

sealed packets, and then loaded into the Costech zero-blank autosampler of the EA, which was

purged with ultra-pure helium for 5 min. The tin cups were then dropped into the EA oven set at

1000°C, flash combusted and then subsequently oxidized and reduced to CO2 and N2. These

gases were separated on a GC column before passing into the IRMS for isotopic measurement.

An L-alanine standard of known isotopic composition (δ13C = -23.33‰, δ15N = -5.56‰, Iso-

Analytical) was used to calibrate the bulk isotopic values measured for the meteorite sample.

Carbon and nitrogen abundances were calculated by comparison of peak areas from the

meteorite data with calibration curves of peak areas from known quantities of acetanilide. Errors

for both abundances and isotopic values are standard deviations for triplicate measurements.

2.17. Gas Chromatography Mass Spectrometry

Two Sutter’s Mill fragments were analyzed for soluble organic compounds by Gas

Chromatography-Mass Spectrometry (GC-MS) of their water and solvent extracts at Arizona

State University. 300 mg of SM2 were powdered in agate mortar, divided in two portions of 100

64

and 200 mg each and extracted in evacuated vials with, respectively, tripled distilled water and

distilled dichlromethane/methanol (9:1 v:v) at 100ºC for 24 hours. A 1.2 g SM12 stone was

chiseled into five fragments of approximate equal weight and incremental distance from the

crust; these were powdered and extracted in sequence with water and solvent (same conditions as

above).

The water extracts were dried cryogenically for the transfer of possible ammonia and amines

(104) and then processed through (+) cation and (-) anion exchange resins for the separation and

collection of amino acids, hydroxyacids and dicarboxylic acids, as described before (e.g., 105).

Results for amino acids, a report of their decreased abundances with depth of the SM stone

suggesting contamination for most as well as the searches of other water-soluble compounds are

described in the main text. It should be noted here that the fragments of Sutter’s Mill that we

analyzed have been the only carbonaceous chondrite samples between those investigated so far

not to release free or bound ammonia (104).

Fig. S34. Single ion GC-MS chromatogram of the aromatic hydrocarbons and sulfur detected in a SM2

solvent extract. Shown are naphthalene (m/z 128), two sets of its higher homologs, methyl- and

dimethylnaphthalenes (m/z 142 and 156), a phthalate, antracene and/or phenanthrene (m/z 178), and

octatomic sulfur (m/z 64).

The GC-MS analyses of a SM2 dichloromethane/methanol extract are shown in Fig. S34.

The amounts of hydrocarbons detected in all SM samples were low and naphthalene was the

most abundant compound, varying between samples 2-10 nanomoles/g. Besides the compounds

shown, we also recognized in SM2 alkyl hydrocarbons but contamination was likely their source

as they were found only as linear species, within a narrow range, 15ºC to 22ºC, and included

65

phytane and two phthalates, known contaminants. The anthracene and/or phenanthrene shown in

Fig. S34 was also a contaminant, as it was not found in interior SM12 fragments.

2.18. Thermoluminescence

Fig. S35. Single Thermoluminescence (TL) glow curves (a) for Sutter’s Mill fragment SM2-1d, identified

in (b). The luminescence produced (normalized to the TL induced intensity of the Dhajala meteorite

which is used as a standard) is plotted against the temperature to which the sample is heated in the

laboratory. The signal from the “as received” sample is termed “natural TL” while the signal produced by

the sample after heating to 500ºC to remove the natural signal and then exposing to a 250 mCi 90Sr beta

source for three minutes is termed the “induced TL”. Also shown is the black-body curve produced by

the sample after its natural TL signal has been removed.

Thermoluminescence (TL) measurements were made using two separate 4 mg aliquots of

SM2-1d, located 0.7-1.0 cm below the remaining fusion crust on fragment SM2-1 (Fig. S35).

The samples were examined under the optical microscope, crushed with a pestle and mortar to

~200µm grains, and placed on 5-mm diameter copper pans for TL measurement. The TL was

measured in the as received state ("natural TL") and after being irradiated by a dose of beta

particles from a 250 mCi 90Sr source ("induced TL"). The TL signal was measured on a

Daybreak Nuclear and Medical TL instrument, modified to bring the sample closer to the

detector, to screen off unwanted black body from the heating strip, and to incorporate a shutter so

the detector (an EMI 96354Q PMT) remains on throughout the experiments. The resulting "glow

66

curves" (plots of TL produced as a function of heating temperature in the laboratory) are shown

in Fig. S35, along with the black body (background) curve. A weak but readily detectable signal

was observed (S/N ~ 10) for Sutter's Mill in both the natural and induced states. This is unusual

since the CM chondrites measured to date had no detectable TL signal. While the induced curve

was broad and hummocky, and extended to low heating temperatures, the natural curve consisted

of TL only in the higher temperature regions of the glow curve.

Fig. S36. Plot of the ratio of the natural TL to the induced TL as a function of glow curve temperature.

Stepwise laboratory heating causes loss of low temperature TL in a way dependent on the heating

temperature (a). The position of the step in the Sutter’s Mill data (b) suggests that this meteorite has been

heated to ~300ºC.

A ratio of natural TL to induced TL, referred to as the plateau curve (Fig. S36), shows a step

at 300±20ºC, suggesting that these two samples of meteorite had been heated to about 300ºC and

had not had time for their TL to recover (estimated to take ~0.2 My). This heating event may

have been due to passage through the Earth's atmosphere, when temperatures as high as 300ºC

may have reached 5-6 mm into the meteorite, although other heating events in the past ~0.2 My,

such as recent solar or impact heating, cannot be excluded. The shape and the intensity of the

induced TL curve resembles those commonly observed for low petrologic type chondrites (say

3.0-3.1) of the ordinary, CV, and CO classes, but is not identical to anything seen before. This

suggests that Sutter's Mill is a unique low petrologic grade chondrite.

67

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